Cooling Flows and Metallicity Gradients in Clusters of Galaxies

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Abstract
The X-ray emission by hot gas at the centers of clusters of galaxies is commonly modeled assuming the existence of steady state, inhomogeneous cooling flows. We derive the metallicity profiles of the intracluster medium expected from such models. The inflowing gas is chemically enriched by Type Ia supernovas and stellar mass loss in the outer parts of the central galaxy, which may give rise to a substantial metallicity gradient. The amplitude of the expected metallicity enhancement toward a cluster's center is proportional to the ratio of the central galaxy's luminosity to the mass-inflow rate. The metallicity of the hotter phases is expected to be higher than that of the colder, denser phases. The metallicity profile expected for the Centaurus Cluster is in good agreement with the metallicity gradient recently inferred from ASCA measurements. However, current data do not rule out alternative models in which cooling is balanced by some heat source. The metallicity gradient does not need to be present in all clusters, depending on the recent merger history of the gas around the central cluster galaxy and on the ratio of the stellar mass in the central galaxy to the gas mass in the cooling flow.
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