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Relativistic plasma and ICM/radio source interaction

Published online by Cambridge University Press:  08 June 2011

Luigina Feretti ,
Gabriele Giovannini ,
Federica Govoni  and
Matteo Murgia
Luigina Feretti
Affiliation:
INAF Istituto di Radioastronomia, Via P. Gobetti n. 101, 40129 Bologna, Italy email: [email protected]
Gabriele Giovannini
Affiliation:
INAF Istituto di Radioastronomia, Via P. Gobetti n. 101, 40129 Bologna, Italy email: [email protected] Dipartimento di Astronomia, Universitá di Bologna, via Ranzani n.1, 40127 Bologna, Italy
Federica Govoni
Affiliation:
INAF Osservatorio Astronomico di Cagliari, Strada 54, Loc. Poggio dei Pini, 09012 Capoterra, Italy
Matteo Murgia
Affiliation:
INAF Osservatorio Astronomico di Cagliari, Strada 54, Loc. Poggio dei Pini, 09012 Capoterra, Italy
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Abstract

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The first detection of a diffuse radio source in a cluster of galaxies, dates back to the 1959 (Coma Cluster, Large et al. 1959). Since then, synchrotron radiating radio sources have been found in several clusters, and represent an important cluster component which is linked to the thermal gas. Such sources indicate the existence of large scale magnetic fields and of a population of relativistic electrons in the cluster volume. The observational results provide evidence that these phenomena are related to turbulence and shock-structures in the intergalactic medium, thus playing a major role in the evolution of the large scale structure in the Universe. The interaction between radio sources and cluster gas is well established in particular at the center of cooling core clusters, where feedback from AGN is a necessary ingredient to adequately describe the formation and evolution of galaxies and host clusters.

Keywords

galaxies: clusters: generalcooling flowsintergalactic mediummagnetic fieldsradio continuum: generalradiation mechanisms: nonthermal
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 340 - 347
Copyright
Copyright © International Astronomical Union 2011

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