New scaling relations in cluster radio halos and the re-acceleration model

Details New scaling relations in cluster radio halos and the re-acceleration model New scaling relations in cluster radio halos and the re-acceleration model

2007-04-26

arxiv.org/abs/0704.3490v1

Mon.Not.Roy.Astron.Soc.378:1565-1574,2007

Astronomy and Astrophysics

Astrophysics

11 pages, 12 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2007.11901.x

In this paper we derive new expected scaling relations for clusters with giant radio halos in the framework of the re-acceleration scenario in a simplified, but physically motivated, form, namely: radio power (P_R) vs size of the radio emitting region (R_H), and P_R vs total cluster mass (M_H) contained in the emitting region and cluster velocity dispersion (sigma_H) in this region. We search for these correlations by analyzing the most recent radio and X-ray data available in the literature for a well known sample of clusters with giant radio halos. In particular we find a good correlation between P_R and R_H and a very tight ``geometrical'' scaling between M_H and R_H. From these correlations P_R is also expected to scale with M_H and sigma_H and this is confirmed by our analysis. We show that all the observed trends can be well reconciled with expectations in the case of a slight variation of the mean magnetic field strength in the radio halo volume with M_H. A byproduct correlation between R_H and sigma_H is also found, and can be further tested by optical studies. In addition, we find that observationally R_H scales non-linearly with the virial radius of the host cluster, and this immediately means that the fraction of the cluster volume which is radio emitting increases with cluster mass and thus that the non-thermal component in clusters is not self-similar.

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