Spectral Energy Distributions of 3C 279 Revisited:BeppoSAXObservations and Variability Models | Zendy

L. Ballo | Zendy; L. Maraschi | Zendy; F. Tavecchio | Zendy; A. Celotti | Zendy; G. Fossati | Zendy; G. Ghisellini | Zendy; E. Pian | Zendy; C. M. Raiteri | Zendy; G. Tagliaferri | Zendy; A. Treves | Zendy; C. M. Urry | Zendy; M. Villata | Zendy

AI Assistant Blog Pricing

Home ZAIA Blog

Open Access

Spectral Energy Distributions of 3C 279 Revisited:BeppoSAXObservations and Variability Models

Author(s) -

L. Ballo,

L. Maraschi,

F. Tavecchio,

A. Celotti,

G. Fossati,

G. Ghisellini,

E. Pian,

C. M. Raiteri,

G. Tagliaferri,

A. Treves,

C. M. Urry,

M. Villata

Publication year - 2002

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/338387

Subject(s) - observatory , physics , astrophysics , spectral energy distribution , egret , jet (fluid) , astronomy , space observatory , light curve , lorentz factor , infrared , gamma ray , lorentz transformation , galaxy , thermodynamics , classical mechanics

We present the BeppoSAX observations of 3C 279 performed in 1997 January13-23 simultaneously with gamma-ray pointings with EGRET on board CGRO andoptical observations at the Torino Observatory (1997 January 11-18). ISO dataclose to this epoch are also available. We compare the derived Spectral EnergyDistribution with those obtained at all other epochs with adequatemultiwavelength coverage. Simple spectral models fitted to the multiepoch SEDssuggest that changes in intensity can be ascribed mainly to the variation ofthe bulk Lorentz factor of the plasma in the jet.Comment: 34 pages (draft format), 6 figures, Accepted for publication in Ap

The content you want is available to Zendy users.

Already have an account? Click here to sign in.

Having issues? You can contact us here

Accelerating Research