The spectral energy distribution of fermi bright blazars
| Title: | The spectral energy distribution of fermi bright blazars |
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| Authors: | Abdo AA; Ackermann M; Agudo I; Ajello M; Aller HD; Aller MF; Angelakis E; Arkharov AA; Axelsson M; Bach U; Baldini L; Ballet J; Barbiellini G; Bastieri D; Baughman BM; Bechtol K; Bellazzini R; Benitez E; Berdyugin A; Berenji B; Blandford RD; Bloom ED; Boettcher M; Bonamente E; Borgland AW; Bregeon J; Brez A; Brigida M; Bruel P; Burnett TH; Burrows D; Buson S; Caliandro GA; Calzoletti L; Cameron RA; Capalbi M; Caraveo PA; Carosati D; Casandjian JM; Cavazzuti E; Cecchi C; Celik O; Charles E; Chaty S; Chekhtman A; Chen WP; Chiang J; Chincarini G; Ciprini S; Claus R; Cohen Tanugi J; Colafrancesco S; Cominsky LR; Conrad J; Costamante L; Cutini S; D'ammando F; Deitrick R; D'Elia V; Dermer CD; de Angelis A; de Palma F; Digel SW; Donnarumma I; Silva EDE; Drell PS; Dubois R; Dultzin D; Dumora D; Falcone A; Farnier C; FAVUZZI, Cecilia; Fegan SJ; Focke WB; Forne E; Fortin P; Frailis M; Fuhrmann L; Fukazawa Y; Funk S; Fusco P; Gomez JL; Gargano F; Gasparrini D; Gehrels N; Germani S; Giebels B; GIGLIETTO, Nicola; Giommi P; Giordano F; Giuliani A; Glanzman T; Godfrey G; Grenier IA; Gronwall C; Grove JE; Guillemot L; Guiriec S; Gurwell MA; Hadasch D; Hanabata Y; Harding AK; Hayashida M; Hays E; Healey SE; Heidt J; Hiriart D; Horan D; Hoversten EA; Hughes RE; Itoh R; Jackson MS; Johannesson G; Johnson AS; Johnson WN; Jorstad SG; Kadler M; Kamae T; Katagiri H; Kataoka J; Kawai N; Kennea J; Kerr M; Kimeridze G; Knodlseder J; Kocian ML; Kopatskaya EN; Koptelova E; Konstantinova TS; Kovalev YY; Kovalev YA; Kurtanidze OM; Kuss M; Lande J; Larionov VM; Latronico L; Leto P; Lindfors E; Longo F; Loparco F; Lott B; Lovellette MN; Lubrano P; Madejski GM; Makeev A; Marchegiani P; Marscher AP; Marshall F; Max Moerbeck W; Mazziotta MN; McConville W; McEnery JE; Meurer C; Michelson PF; Mitthumsiri W; Mizuno T; Moiseev AA; Monte C; Monzani ME; Morselli A; Moskalenko IV; Murgia S; Nestoras I; Nilsson K; Nizhelsky NA; Nolan PL; Norris JP; Nuss E; Ohsugi T; Ojha R; Omodei N; Orlando E; Ormes JF; Osborne J; Ozaki M; Pacciani L; Padovani P; Pagani C; Page K; Paneque D; Panetta JH; Parent D; Pasanen M; Pavlidou V; Pelassa V; Pepe M; Perri M; Pesce Rollins M; Piranomonte S; Piron F; Pittori C; Porter TA; Puccetti S; Rahoui F; Raino S; Raiteri C; Rando R; Razzano M; Reimer A; Reimer O; Reposeur T; Richards JL; Ritz S; Rochester LS; Rodriguez AY; Romani RW; Ros JA; Roth M; Roustazadeh P; Ryde F; Sadrozinski HFW; Sadun A; Sanchez D; Sander A; Parkinson PMS; Scargle JD; Sellerholm A; Sgro C; Shaw MS; Sigua LA; Siskind EJ; Smith DA; Smith PD; Spandre G; Spinelli P; Starck JL; Stevenson M; Stratta G; Strickman MS; Suson DJ; Tajima H; Takahashi H; Takahashi T; Takalo LO; Tanaka T; Thayer JB; Thayer JG; Thompson DJ; Tibaldo L; Torres DF; Tosti G; Tramacere A; Uchiyama Y; Usher TL; Vasileiou V; Verrecchia F; Vilchez N; Villata M; Vitale V; Waite AP; Wang P; Winer BL; Wood KS; Ylinen T; Zensus JA; Zhekanis GV; Ziegler M. |
| Contributors: | Abdo, Aa; Ackermann, M; Agudo, I; Ajello, M; Aller, Hd; Aller, Mf; Angelakis, E; Arkharov, Aa; Axelsson, M; Bach, U; Baldini, L; Ballet, J; Barbiellini, G; Bastieri, D; Baughman, Bm; Bechtol, K; Bellazzini, R; Benitez, E; Berdyugin, A; Berenji, B; Blandford, Rd; Bloom, Ed; Boettcher, M; Bonamente, E; Borgland, Aw; Bregeon, J; Brez, A; Brigida, M; Bruel, P; Burnett, Th; Burrows, D; Buson, S; Caliandro, Ga; Calzoletti, L; Cameron, Ra; Capalbi, M; Caraveo, Pa; Carosati, D; Casandjian, Jm; Cavazzuti, E; Cecchi, C; Celik, O; Charles, E; Chaty, S; Chekhtman, A; Chen, Wp; Chiang, J; Chincarini, G; Ciprini, S; Claus, R; Cohen Tanugi, J; Colafrancesco, S; Cominsky, Lr; Conrad, J; Costamante, L; Cutini, S; D'Ammando, F; Deitrick, R; D'Elia, V; Dermer, Cd; de Angelis, A; de Palma, F; Digel, Sw; Donnarumma, I; Silva, Ede; Drell, P; Dubois, R; Dultzin, D; Dumora, D; Falcone, A; Farnier, C; Favuzzi, Cecilia; Fegan, Sj; Focke, Wb; Forne, E; Fortin, P; Frailis, M; Fuhrmann, L; Fukazawa, Y; Funk, S; Fusco, P; Gomez, Jl; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giebels, B; Giglietto, Nicola; Giommi, P; Giordano, F; Giuliani, A; Glanzman, T; Godfrey, G; Grenier, Ia; Gronwall, C; Grove, Je; Guillemot, L; Guiriec, S; Gurwell, Ma; Hadasch, D |
| Publication Year: | 2010 |
| Collection: | Politecnico di Bari: Iris POLIBA (Catalogo dei prodotti della Ricerca) |
| Subject Terms: | BL Lacertae objects: generalGalaxies: activeGamma rays: galaxiesQuasars: generalRadiation mechanisms: non-thermal |
| Description: | We have conducted a detailed investigation of the broadband 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 3 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 broadband 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 SED 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 broadband colors (i.e., the radio to optical, alpha(ro), and optical to X-ray, alpha(ox), spectral slopes) and from the gamma-ray spectral index. Our data show that the synchrotron peak frequency (nu(S)(peak)) is positioned between 10(12.5) and 10(14.5) Hz in broad-lined flat spectrum radio quasars (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 SED, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. More complex models involving external Compton radiation or multiple SSC components are required to reproduce the overall SED and the observed spectral variability. While more than 50% of known radio bright high energy peaked (HBL) BL Lacs are detected in ... |
| Document Type: | article in journal/newspaper |
| File Description: | STAMPA |
| Language: | English |
| Relation: | info:eu-repo/semantics/altIdentifier/wos/WOS:000277960000002; volume:716; issue:1; firstpage:30; lastpage:70; numberofpages:41; journal:THE ASTROPHYSICAL JOURNAL; https://hdl.handle.net/11589/5230 |
| DOI: | 10.1088/0004-637X/716/1/30 |
| DOI: | 10.1088/0004-637X/716/1/30/meta |
| Availability: | https://hdl.handle.net/11589/5230; https://doi.org/10.1088/0004-637X/716/1/30; http://iopscience.iop.org/article/10.1088/0004-637X/716/1/30/meta |
| Rights: | info:eu-repo/semantics/openAccess ; license:Tutti i diritti riservati |
| Accession Number: | edsbas.2A21A7D6 |
| Database: | BASE |