Volume 396, Number 1, December II 2002
|Page(s)||83 - 89|
|Section||Cosmology (including clusters of galaxies)|
|Published online||22 November 2002|
The radio luminosity function of cluster radio halos
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, Postfach 1317, 85741 Garching, Germany
2 Sterrewacht, Oort Gebouw, PO Box 9513, 2300 RA Leiden, The Netherlands
Corresponding author: T. A. Enßlin, email@example.com
Accepted: 11 September 2002
A significant fraction of galaxy clusters exhibits cluster-wide radio halos. We give a simple prediction of the local and higher redshift radio halo luminosity function (RHLF) on the basis of (i) an observed and a theoretical X-ray cluster luminosity function (XCLF) (ii) the observed radio–X-ray luminosity correlation (RXLC) of galaxy clusters with radio halos (iii) an assumed fraction of galaxy clusters to have radio halos as supported by observations. We then find 300–700 radio halos with mJy, and 105–106 radio halos with Jy should be visible on the sky. 14% of the mJy and 56% of the Jy halos are located at . Subsequently, we give more realistic predictions taking into account (iv) a refined estimate of the radio halo fraction as a function of redshift and cluster mass, and (v) a decrease in intrinsic radio halo luminosity with redshift due to increased inverse Compton electron energy losses on the Cosmic Microwave Background (CMB). We find that this reduces the radio halo counts from the simple prediction by only 30 % totally, but the high redshift () counts are more strongly reduced by 50–70%. These calculations show that the new generation of sensitive radio telescopes, including LOFAR, ATA, EVLA, SKA and the already-operating GMRT should be able to detect large numbers of radio halos and will provide unique information for studies of galaxy cluster merger rates and associated non-thermal processes.
Key words: X-rays: galaxies: clusters / radiation mechanism: non-thermal / radio continuum: general / galaxies: intergalactic medium / galaxies: cluster: general
© ESO, 2002
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