A Simple Physical Model for the Gas Distribution in Galaxy Clusters

Abstract

The dominant baryonic component of galaxy clusters is hot gas whose distribution is commonly probed through X-ray emission arising from thermal bremsstrahlung. The density profile thus obtained has been traditionally modeled with a beta-profile, a simple function with only three parameters. However, this model is known to be insufficient for characterizing the range of cluster gas distributions, and attempts to rectify this shortcoming typically introduce additional parameters to increase the fitting flexibility. We use cosmological and physical considerations to obtain a family of profiles for the gas with fewer parameters than the beta-model but which better accounts for observed gas profiles over wide radial intervals.

8 pages, 5 figures, accepted for publication in ApJ Letters

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• A Study of Gas Entropy Profiles of 47 Galaxy Clusters and Groups Out to the Virial Radius
• Bound on the graviton mass from Chandra X-ray cluster sample
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• Optical inverse-Compton emission from clusters of galaxies
• Virial theorem in clusters of galaxies with MOND
• The mass and galaxy distribution around SZ-selected clusters
• Predicting the Scaling Relations between the Dark Matter Halo Mass and Observables from Generalised Profiles II: Intracluster Gas Emission
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