Cluster soft excess emission in the XMM/Newton era

Details Cluster soft excess emission in the XMM/Newton era Cluster soft excess emission in the XMM/Newton era

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..330l&link_type=abstract

In: Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 J

Astronomy and Astrophysics

Astronomy

Galaxy Clusters

Scientific paper

In the XMM Newton era research on the topic of cluster soft excess takes a sharp upward turn. The phenomenon is clearly confirmed for many clusters moreover its thermal warm gas origin is established for the outer parts of five clusters through the detection of O VII emission at the cluster redshift. Since this line is not present in the inner soft excess spectra the warm gas may reside in filaments projecting from a cluster and accounting in total for a lot of `missing baryons'. Nonetheless the mystery of the inner soft excess which is bright enough to remain clearly visible even in the cooling flow regions where the hot intracluster medium is very luminous can only be explained as inverse Compton emission. By using the clusters A1795 and AS1101 as test cases we modeled the central soft excesses with a power law and in this way evaluated the observed cosmic rays pressure. In each case the parameter values indicate that the pressure is at least sufficient for equipartition between cosmic rays and gas. Thus there is compelling evidence that the soft excess emission in clusters centers and the cooling flow riddle are really one and the same problem.

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