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Superluminal Motion in the Gamma-Ray Blazar 3C 279

Published online by Cambridge University Press:  12 April 2016

S.C. Unwin ,
A.E. Wehrle ,
W. Xu ,
A.C. Zook  and
A.P. Marscher
S.C. Unwin
Affiliation:
Jet Propulsion Laboratory, Caltech, Pasadena, CA, U.S.A.
A.E. Wehrle
Affiliation:
IPAC, Jet Propulsion Laboratory, Caltech, Pasadena, CA, U.S.A.
W. Xu
Affiliation:
IPAC, Jet Propulsion Laboratory, Caltech, Pasadena, CA, U.S.A.
A.C. Zook
Affiliation:
Pomona College, Claremont, CA, U.S.A.
A.P. Marscher
Affiliation:
Boston University, Boston, MA, U.S.A.

Abstract

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The blazar 3C 279 is one of the strongest extragalactic sources of γ-rays, and is also one of the best studied superluminal radio sources. Definitive testing of models of the broad-band spectral energy distribution, especially in the X-ray and γ-ray regions requires knowledge of the evolution of the spectrum with time. Within the context of the relativistic jet model, multi-wavelength monitoring of the parsec-scale radio jet is also required. We present here the first steps toward such a test, using extensive VLBI monitoring over a 13 year interval at 22 GHz, and γ-ray observations between 1991 and 1996.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 69 - 70
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

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Wehrle, A.E., et al. 1997. ApJ, submitted.Google Scholar