Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-28T21:43:19.202Z Has data issue: false hasContentIssue false
  • English
  • Français

IGM Heating and AGN activity in Fossil Galaxy Groups

Published online by Cambridge University Press:  25 July 2014

H. Miraghaei ,
H. G. Khosroshahi ,
H.-R. Klöckner ,
T. J. Ponman ,
N. N. Jetha  and
S. Raychaudhury
H. Miraghaei
Affiliation:
Department of Physics, Sharif University of Technology PO Box 11365-9161, Tehran, Iran email: [email protected] School of Astronomy, Institute for Research in Fundamental Sciences, PO Box 19395-5531, Tehran, Iran
H. G. Khosroshahi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences, PO Box 19395-5531, Tehran, Iran
H.-R. Klöckner
Affiliation:
Subdepartment of Astrophysics, University of Oxford, Denys-Wilkinson Building, Keble Road, Oxford, OX1 3RH, UK Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
T. J. Ponman
Affiliation:
School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
N. N. Jetha
Affiliation:
Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35805, USA
S. Raychaudhury
Affiliation:
School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
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.

Fossil galaxy groups are energetically and morphologically ideal environments to study the intergalactic medium (IGM) heating, because their inter-galactic gas is undisturbed due to the lack of recent group scale mergers. We study the role of active galactic nuclei (AGN) in heating the IGM in a sample of five fossil galaxy groups by employing properties at 610 MHz and 1.4 GHz. We find that two of the dominant galaxies in fossil groups, ESO 3060170 and RX J1416.4+2315, are associated with the radio lobes. We evaluate the PdV work of the radio lobes and their corresponding heating power and compare to the X-ray emission loss within cooling radius. Our results show that the power due to mechanical heating is not sufficiently high to suppress the cooling.

Keywords

galaxies: activegalaxies: clusters: generalintergalactic mediumcooling flowsradio continuum: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S304: Multiwavelength AGN Surveys and Studies , October 2013 , pp. 349 - 350
Copyright
Copyright © International Astronomical Union 2014 

References

Bîrzan, L., Rafferty, D. A., McNamara, B. R., Wise, M. W. & Nulsen, P. E. J. 2004, ApJ, 607, 800Google Scholar
Jones, L. R., Ponman, T. J., Horton, A., Babul, A., Ebeling, H. & Burke, D. J. 2003, MNRAS, 343, 627Google Scholar
Peterson, J. R. & Fabian, A. C. 2006, Phys. Rep., 427, 1CrossRefGoogle Scholar
Gitti, M., Brighenti, F. & McNamara, B. R. 2012, Adv. Astron., 2012, 1Google Scholar
Jetha, N. N., Hardcastle, M. J., Babul, A., O'Sullivan, E., Ponman, T. J., Raychaudhury, S., & Vrtilek, J. 2008, MNRAS, 384, 1344CrossRefGoogle Scholar
Khosroshahi, H. G., Ponman, T. J., & Jones, L. R. 2007, MNRAS, 377, 595CrossRefGoogle Scholar