Revisiting the soft X-ray excess emission in clusters of galaxies observed with XMM-Newton

Abstract

We analyze four XMM-Newton galaxy clusters in order to test whether their soft X-ray excess emission in the 0.2-0.5 keV band as reported by Kaastra et al. (2003) maintains after the application of the current knowledge of the XMM-Newton background and calibration. We show that in the bright central 500 kpc regions the details of the background modeling are insignificant. Thus, the cluster soft excess is not a background artifact, contrary to recent claims by Bregman et al. (2006). We find evidence that the change in PN calibration between years 2002 and 2005 results in significant decrease of the soft excess signal. However, the MOS instruments measure significant amounts of soft excess, or sub-Galactic NH. These differences are compatible with the current level of uncertainty in the calibration of both instruments.

arXiv commentApJ in press, minor stylistic changes

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• Possible non-thermal nature of the soft-excess emission in the cluster of galaxies Sersic 159-03
• Soft and hard X-ray excess emission in Abell 3112 observed with Chandra
• The diffuse soft excess emission in the Coma cluster from the ROSAT All-Sky Survey
• Clusters of galaxies: setting the stage
• Suzaku observations of X-ray excess emission in the cluster of galaxies A3112
• Suzaku Constraints on the Soft and Hard Excess Emissions from Abell 2199
• A WHIM origin for the soft excess emission in the Coma cluster
• X-ray emission in IllustrisTNG circum-cluster environments. II -- Possible origins of the soft X-ray excess emission