A good mass proxy for galaxy clusters with XMM-Newton

Abstract

We use a sample of 39 galaxy clusters at redshift z < 0.1 observed by XMM-Newton to investigate the relations between X-ray observables and total mass. Based on central cooling time and central temperature drop, the clusters in this sample are divided into two groups: 25 cool core clusters and 14 non-cool core clusters, respectively. We study the scaling relations of Lbol-M500, M500-T, M500-Mg and M500-YX, and also the influences of cool core on these relations. The results show that the M500-YX relation has a slope close to the standard self-similar value, has the smallest scatter and does not vary with the cluster sample. Moreover, the M500-YX relation is not affected by the cool core. Thus, the parameter of YX may be the best mass indicator.

ApJ Accepted, 25 pages, 7 figures

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• The scaling relations and the fundamental plane for radio halos and relics of galaxy clusters
• The PIPER Survey: I. An Initial Look at the Intergalactic Globular Cluster Population in the Perseus Cluster
• NGC 3314a/b and NGC 3312: Ram pressure stripping in Hydra I Cluster substructure
• A catalog of galaxy clusters identified from SCUSS, SDSS, and unWISE
• Unbiased Correction Relations for Galaxy Cluster properties Derived from Chandra and XMM-Newton
• The ${\mathrm{Y}}_{\mathrm{SZ},\mathrm{Planck}}-{\mathrm{Y}}_{\mathrm{SZ},\mathrm{XMM}}$ scaling relation and its difference between cool-core and non-cool-core clusters