Other
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.3323m&link_type=abstract
American Astronomical Society, HEAD meeting #11, #33.23; Bulletin of the American Astronomical Society, Vol. 41, p.709
Other
Scientific paper
Our comprehensive multi-waveband monitoring program of blazars uses correlations and times lags to determine the locations of gamma-ray flares in the relativistic jets of blazars. Our observations of 33 objects include monitoring of (1) the emission and polarization structure of the jet at 43 GHz with the VLBA, (2) mapping of the finer scale structure at 86 GHz with the GMVA, (3) monitoring of the optical polarization, and (4) densely-sampled light curves at radio, optical/near-IR, X-ray, and gamma-ray frequencies. A number of blazars have already exhibited flares observed in sufficient detail to infer where the high-energy emission arises. Many of the flares are associated with superluminal knots propagating down the jet. A knot produces one or more gamma-ray flares as it travels down the jet toward the compact, stationary bright spot seen on the VLBA images (mm-wave "core"), and also during its passage through the core and as it continues downstream. We infer that the core consists of one or more standing oblique shocks. Some of the flares are caused by an increase in the number of relativistic electrons, while others require rapid changes in the seed photon field as the knot moves down the jet. We use this information plus systematic changes (often rotations) of the optical linear polarization vector to infer the physics of the inner jet regions.
This research was supported in part by NASA through Fermi grants NNX08AV65G and NNX08AV61G and ADP grant NNX08AJ64G, and by NSF grant AST-0907893.
Agudo Iv'an
Aller Hugh D.
Aller Margo F.
Jorstad Svetlana G.
Krichbaum Th.
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