Simultaneous Multiwavelength Spectrum and Variability of 3C 279 from 10 9 to 10 24 Hz

Details Simultaneous Multiwavelength Spectrum and Variability of 3C 279 from 10 9 to 10 24 Hz Simultaneous Multiwavelength Spectrum and Variability of 3C 279 from 10 9 to 10 24 Hz

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...461..698h&link_type=abstract

Astrophysical Journal v.461, p.698

Astronomy and Astrophysics

Astronomy

105

Infrared: Galaxies, Gamma Rays: Observations, Galaxies: Quasars: Individual Alphanumeric: 3C 279, X-Rays: Galaxies

Scientific paper

Data from a number of monitoring programs have been combined with data from the Compton Gamma Ray Observatory and the Ginga X-ray satellite to construct a spectrum covering nearly 15 decades in frequency during or near the time of the 3C 279 γ-ray flare observed by EGRET in 1991 June. A much less complete spectrum is presented for 1991 October. Light curves from early 1991 to mid-1992 are presented for radio, millimeter, submillimeter, infrared, optical, and γ-rays. Although the temporal coverage is incomplete, the only evidence for correlation in variability between the γ-rays and lower frequencies is a flare in the optical R-band that peaks within ~1 day of the maximum in the γ-ray light curve. The variability shows higher relative amplitude in γ-rays than in the R band. We present spectral fits to the overall multi-wave band spectrum averaged over the 1991 June flare corresponding to two models: (i) synchrotron self-Compton (SSC) emission from a relativistic jet and (ii) inverse Compton scattering of seed photons originating external to the jet (ECS) by the synchrotron-emitting relativistic electrons in the jet. Either model can fit the observed spectra satisfactorily. The higher amplitude of the γ-ray variations is as predicted by the SSC model and can be accommodated within the ECS model if the flare is caused by a temporary change in the bulk Lorentz factor of the γ-ray-emitting plasma.

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