Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-14T17:40:59.321Z Has data issue: false hasContentIssue false
  • English
  • Français

Study of the parsec-scale jet in the blazar 3C 66A with VLBA

Published online by Cambridge University Press:  21 February 2013

Guang-Yao Zhao ,
Yong-Jun Chen ,
Zhi-Qiang Shen ,
Hiroshi Sudou ,
Satoru Iguchi ,
Yasuhiro Murata  and
Yoshiaki Taniguchi
Guang-Yao Zhao
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: gyzhao@shao.ac.cn University of Chinese Academy of Sciences, Beijing 100049, China Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Yong-Jun Chen
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: gyzhao@shao.ac.cn Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Zhi-Qiang Shen
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China email: gyzhao@shao.ac.cn Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, China
Hiroshi Sudou
Affiliation:
Faculty of Engineering, Gifu University, Gifu 501-1193, Japan
Satoru Iguchi
Affiliation:
National Astronomical Observatory of Japan, Tokyo 181-8588, Japan
Yasuhiro Murata
Affiliation:
The Institute of Space and Astronautical Science, JAXA, Kanagawa 229-8510, Japan
Yoshiaki Taniguchi
Affiliation:
Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama 790-8577, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report 4-epoch VLBA observations of 3C 66A at 22GHz. The resulting images show a typical core-jet structure. We combine our results with some previous results to investigate the proper motions of the jet components. The kinematics of 3C 66A is quite complicated; mildly superluminal motions as well as apparent inward motions have been detected for some components. The inward motions may imply position change of the observed core.

Keywords

Radio continuum: galaxies— galaxies: individual (3C 66A)— galaxies: jet
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 367 - 368
Copyright
Copyright © International Astronomical Union 2013

References

Abdo, A. A., Ackermann, M., Agudo, I.et al. 2010, ApJ, 716, 30Google Scholar
Britzen, S., Vermeulen, R. C., Campbell, R. M.et al. 2008, A&A, 484, 119Google Scholar
Cai, H.-B., Shen, Z.-Q., Sudou, H.et al. 2007, A&A 468 963 (C07)Google Scholar
Jorstad, S. G., Marscher, A. P., Mattox, J. R.et al. 2001, ApJS 134 181 (J01)CrossRefGoogle Scholar
Jorstad, S. G., Marscher, A. P., Lister, M. L., et al. 2005, AJ 130 1418 (J05)CrossRefGoogle Scholar
Marscher, A. P., Jorstad, S. G., Mattox, J. R., Wehrle, A. E. 2002, ApJ, 577, 85Google Scholar
Sudou, H., Iguchi, S. 2011, AJ, 142, 49CrossRefGoogle Scholar