Abstract
Abstract We investigate the possible existence and X-ray emission of warm gas associated with the gravitational potential wells of individual galaxies in rich clusters in an attempt to account for the EUV and soft X-ray excess detected in some nearby clusters. The intrinsic properties of hot intracluster gas and warm galactic gas are specified by the assumption of isothermality and the equation of hydrostatic equilibrium, and the underlying gravitational potentials are described by the universal density profile. Moreover, the Schechter luminosity function and the King model are adopted for the number and spatial distributions of the cluster galaxies, respectively. We fix the gas fraction in different galaxies using Einstein Observatory and ROSAT observations. Our numerical calculation in conjunction with Monte Carlo technique shows that cluster galaxies consisting primarily of ellipticals can make a nonnegligible contribution to the EUV and soft X-ray emission seen in the central regions of clusters. For a rich cluster, like Coma, a small fraction (6%) of soft X-ray emission in the 0.1–1 keV band may come from galaxies, while a significant excess of up to 26% in the 0.01–0.1 keV band can be attributed to galaxies. The cosmological implications and observational consequence of this alternative scenario for the EUV and soft X-ray excess in clusters are addressed.
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