The power spectrum amplitude from clusters revisited: σ_8 using simulations with preheating and cooling

Details The power spectrum amplitude from clusters revisited: σ_8 using simulations with preheating and cooling The power spectrum amplitude from clusters revisited: σ_8 using simulations with preheating and cooling

2002-11-05

arxiv.org/abs/astro-ph/0211090v3

Mon.Not.Roy.Astron.Soc. 346 (2003) 319

Astronomy and Astrophysics

Astrophysics

9 pages LaTeX file using mn2e.cls, with seven figures incorporated. Modest updates from version 2 to match version accepted by

Scientific paper

10.1046/j.1365-2966.2003.07088.x

The amplitude of density perturbations, for the currently-favoured LambdaCDM cosmology, is constrained using the observed properties of galaxy clusters. The catalogue used is that of Ikebe et al. (2002). The cluster temperature to mass relation is obtained via N-body/hydrodynamical simulations including radiative cooling and preheating of cluster gas, which we have previously shown to reproduce well the observed temperature--mass relation in the innermost parts of clusters (Thomas et al. 2002). We generate and compare mock catalogues via a Monte Carlo method, which allows us to constrain the relation between X-ray temperature and luminosity, including its scatter, simultaneously with cosmological parameters. We find a luminosity-temperature relation in good agreement with the results of Ikebe et al. (2002), while for the matter power spectrum normalization, we find $\sigma_8 = 0.78_{-0.06}^{+0.30}$ at 95 per cent confidence for $\Omega_0 = 0.35$. Scaling to WMAP's central value of $\Omega_0 = 0.27$ would give a best-fit value of $\sigma_8 \simeq 0.9$.

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