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Astrophysical Journal 716 (2010) 30-70
The Spectral Energy Distribution of Fermi bright blazars
A.A. Abdo, M. Ackermann, M. Ajello, M. Axelsson, L. Baldini, J. Ballet1, G. Barbiellini, D. Bastieri, B.M. Baughman, K. Bechtol, R. Bellazzini, B. Berenji, R.D. Blandford, E.D. Bloom, E. Bonamente, A. Borgland, J. Bregeon, A. Brez, M. Brigida, P. Bruel2, T. H. Burnett, S. Buson, G. A. Caliandro, R. A. Cameron, P. A. Caraveo, J. M. Casandjian1, E. Cavazzuti, C. Cecchi, O. Celik, E. Charles1, S. Chaty1, A. Chekhtman, J. Chiang, S. Ciprini, R. Claus, J. Cohen-Tanugi3, S. Colafrancesco, L. R. Cominsky, J. Conrad, L. Costamante, S. Cutini, C. D. Dermer, A. De Angelis, F. De Palma, S. W. Digel, E. do Couto e Silva, P. S. Drell, R. Dubois, D. Dumora4, C. Farnier3, C. Favuzzi, S. J. Fegan2, W. B. Focke, P. Fortin2, M. Frailis, L. Fuhrmann, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Gehrels, S. Germani, B. Giebels2, N. Giglietto, P. Giommi, F. Giordano, T. Glanzman, G. Godfrey, I. A. Grenier1, J. E. Grove, L. Guillemot4, S. Guiriec, D. Hadasch, Y. Hanabata, A. K. Harding, M. Hayashida, E. Hays, S. E. Healey, D. Horan2, R. E. Hughes, R. Itoh, M. S. Jackson, G. Johannesson, A. S. Johnson, W. N. Johnson, M. Kadler, T. Kamae, H. Katagiri, J. Kataoka, N. Kawai, M. Kerr, J. Knodlseder5, M. L. Kocian, M. Kuss, J. Lande, L. Latronico, F. Longo, F. Loparco, B. Lott4, M. N. Lovellette, P. Lubrano, G. M. Madejski, A. Makeev, W. Max-Moerbeck, M. N. Mazziotta, W. Mcconville, J. E. McEnery, C. Meurer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko, S. Murgia, I. Nestoras, K. Nilsson, N. A. Nizhelsky, P. L. Nolan, J. P. Norris, E. Nuss3, T. Ohsugi, R. Ojha, N. Omodei, E. Orlando, J. F. Ormes, J. Osborne, M. Ozaki, L. Pacciani, P. Padovani, C. Pagani, K. Page, D. Paneque, J. H. Panetta, D. Parent4, M. Pasanen, V. Pavlidou, V. Pelassa3, M. Pepe, M. Perri, M. Pesce-Rollins, S. Piranomonte, F. Piron3, C. Pittori, T. A. Porter, S. Puccetti, F. Rahoui1, S. Rainò, C. Raiteri, R. Rando, M. Razzano, A. Reimer, O. Reimer, T. Reposeur4, J. L. Richards, S. Ritz, L. S. Rochester, A. Y. Rodriguez, R. W. Romani, J. A. Ros, M. Roth, P. Roustazadeh, F. Ryde, H. F.-W. Sadrozinski, A. Sadun, D. Sanchez2, A. Sander, P. M. Saz Parkinson, J. D. Scargle, A. Sellerholm, C. Sgrò, M. S. Shaw, L. A. Sigua, E. J. Siskind, D. A. Smith4, P. D. Smith, G. Spandre, P. Spinelli, J.-L. Starck1, M. Stevenson, G. Stratta, M. S. Strickman, D. J. Suson, H. Tajima, H. Takahashi, T. Takahashi, L. O. Takalo, T. Tanaka, J. B. Thayer, J. G. Thayer, D. J. Thompson, L. Tibaldo1, D. F. Torres, G. Tosti, A. Tramacere, Y. Uchiyama, T. L. Usher, V. Vasileiou, F. Verrecchia, N. Vilchez5, M. Villata, V. Vitale, A. P. Waite, P. Wang, B. L. Winer, K. S. Wood, T. Ylinen, J. A. Zensus, G. V. Zhekanis, M. Ziegler

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. (...)
1:  AIM - UMR 7158 - Astrophysique Interactions Multi-échelles
2:  LLR - Laboratoire Leprince-Ringuet
3:  LPTA - Laboratoire de Physique Théorique et Astroparticules
4:  CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
5:  CESR - Centre d'étude spatiale des rayonnements
Sciences of the Universe/Astrophysics/High Energy Astrophysical Phenomena

Physics/Astrophysics/High Energy Astrophysical Phenomena
BL Lacertae objects: general – galaxies: active – gamma rays: galaxies – quasars: general – radiation mechanisms: non-thermal
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