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Interaction of Cygnus A with its environment

Published online by Cambridge University Press:  24 March 2015

Paul E. J. Nulsen ,
Andrew J. Young ,
Ralph P. Kraft ,
Brian R. McNamara  and
Michael W. Wise
Paul E. J. Nulsen
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA email: pnulsen@cfa.harvard.edu, rkraft@cfa.harvard.edu
Andrew J. Young
Affiliation:
School of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK email: andy.young@bristol.ac.uk
Ralph P. Kraft
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA email: pnulsen@cfa.harvard.edu, rkraft@cfa.harvard.edu
Brian R. McNamara
Affiliation:
Department of Physics and Astronomy, University of Waterloo, 200 University Avenue West, Waterloo, Ontario, CanadaN2L 3G1 email: mcnamara@uwaterloo.ca
Michael W. Wise
Affiliation:
ASTRON, Netherlands Institute for Radio Astronomy P.O. Box 2, 7990 AA Dwingeloo, Netherlands email: wise@astron.nl
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Abstract

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Cygnus A, the nearest truly powerful radio galaxy, resides at the centre of a massive galaxy cluster. Chandra X-ray observations reveal its cocoon shocks, radio lobe cavities and an X-ray jet, which are discussed here. It is argued that X-ray emission from the outer regions of the cocoon shocks is nonthermal. The X-ray jets are best interpreted as synchrotron emission, suggesting that they, rather than the radio jets, are the path of energy flow from the nucleus to the hotspots. In that case, a model shows that the jet flow is non-relativistic and carries in excess of one solar mass per year.

Keywords

radio continuum: galaxiesX-rays: galaxies: clustersgalaxies: individual (Cygnus A)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S313: Extragalactic jets from every angle , September 2014 , pp. 236 - 241
Copyright
Copyright © International Astronomical Union 2015 

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