Mass-temperature relation of galaxy clusters: implications from the observed luminosity-temperature relation and X-ray temperature function
Abstract
We derive constraints on the mass-temperature relation of galaxy clusters from their observed luminosity-temperature relation and X-ray temperature function. Adopting the isothermal gas in hydrostatic equilibrium embedded in the universal density profile of dark matter halos, we compute the X-ray luminosity for clusters as a function of their hosting halo mass. We find that in order to reproduce the two observational statistics, the mass-temperature relation is very tightly constrained as T_{gas} = (1.5~2.0)keV (M_{vir}/10^{14}h_{70}^{-1}M_\odot)^{0.5~0.55}, and a simple self-similar evolution model (T_{gas} \propto M_{vir}^{2/3}) is strongly disfavored. In the cosmological model that we assume (a \Lambda CDM universe with \Omega_0=0.3, \lambda_0=0.7 and h_{70}=1), the derived mass-temperature relation suggests that the mass fluctuation amplitude \sigma_8 is 0.7--0.8.
Cite
@article{arxiv.astro-ph/0212284,
title = {Mass-temperature relation of galaxy clusters: implications from the observed luminosity-temperature relation and X-ray temperature function},
author = {Mamoru Shimizu and Tetsu Kitayama and Shin Sasaki and Yasushi Suto},
journal= {arXiv preprint arXiv:astro-ph/0212284},
year = {2009}
}
Comments
25 pages, 10 figures. Omission of scaling of 1/h**2 in several figures is corrected. Conclusions remain unchanged. ApJ 2003 June 10 issue, in press