Abstract
We describe a multiwavelength program of monitoring of a sample of bright γ-ray blazars, which the Boston University (BU) group has being carrying out since June 2007. The program includes monthly monitoring with the Very Long Baseline Array at 43 GHz, optical photometric and polarimetric observations, construction and analysis of UV and X-ray light curves obtained with the Rossi X-ray Timing Explorer (RXTE) and Swift satellites, and construction and analysis of γ-ray light curves based on data provided by the Large Area Telescope of the Fermi Gamma-ray Space Telescope. We present general results about the kinematics of parsec-scale radio jets, as well as the connection between γ-ray outbursts and jet events.
Highlights
IntroductionDuring the Compton Gamma Ray Observatory operation from 1991 to 2000, the Energetic Gamma
During the Compton Gamma Ray Observatory operation from 1991 to 2000, the Energetic GammaRay Experiment Telescope (EGRET) detected nearly 70 blazars at photon energies of 0.1–3 GeV [1].Energetic GammaRay Experiment Telescope (EGRET) was a predecessor of the Large Area Telescope (LAT) of the Fermi Gamma-Ray SpaceTelescope [2], which was launched in August 2008 and continues to operate at 0.1–300 GeV in survey mode
We are performing a comprehensive program of multi-wavelength monitoring of a sample of γ-ray blazars, the VLBA-Boston University (BU)-BLAZAR program
Summary
During the Compton Gamma Ray Observatory operation from 1991 to 2000, the Energetic Gamma. The BU group examined the coincidence of times of high γ-ray flux and ejections of superluminal components from the core and, despite sparse EGRET γ-ray light curves, found that in ∼50% of events with sufficient VLBA and γ-ray data, γ-ray outbursts can be associated with the appearance of superluminal knots in radio jets [11]. This finding suggested that the γ-ray flares occurred in the parsec-scale regions of the jet rather than closer to the central engine. The program aims to determine the locations and mechanisms of origin of high energy photons in blazars
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