The structural and scaling properties of nearby galaxy clusters - II. The M-T relation

Details The structural and scaling properties of nearby galaxy clusters - II. The M-T relation The structural and scaling properties of nearby galaxy clusters - II. The M-T relation

2005-02-10

arxiv.org/abs/astro-ph/0502210v2

Astron.Astrophys.441:893-903,2005

Astronomy and Astrophysics

Astrophysics

11 pages, 4 figures, A&A in press, updated to match the accepted version (19/08/2005). Minor text clarifications, more detaile

Scientific paper

10.1051/0004-6361:20052856

Using a sample of ten nearby (z< 0.15), relaxed galaxy clusters in the temperature range [2-9] keV, we have investigated the scaling relation between the mass at various density contrasts (delta=2500,1000,500,200) and the cluster temperature. The masses are derived from NFW-type model fits to mass profiles, obtained under the hydrostatic assumption using precise measurements, with XMM, at least down to delta=1000. The logarithmic slope of the M-T relation is well constrained and is the same at all delta, reflecting the self-similarity of the mass profiles. At delta=500, the slope of the relation for the sub-sample of hot clusters (kT>3.5 keV) is consistent with the standard self-similar expectation: alpha= 1.49\pm0.15. The relation steepens when the whole sample is considered: alpha=1.71\pm0.09. The normalisation of the relation is discrepant (by ~ 30%), at all density contrasts, with the prediction from purely gravitation based models. Models that take into account radiative cooling and galaxy feedback are generally in better agreement with our data. We argue that remaining discrepancies, in particular at low delta, are more likely due to problems with models of the ICM thermal structure rather than to an incorrect estimate of the mass from X-ray data.

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