Measuring the Density Fluctuation From the Cluster Gas Mass Function

Abstract

We investigate the gas mass function of clusters of galaxies to measure the density fluctuation spectrum on cluster scales. The baryon abundance confined in rich clusters is computed from the gas mass function and compared with the mean baryon density in the universe which is predicted by the Big Bang Nucleosynthesis. This baryon fraction and the slope of the gas mass function put constraints on $σ_8$, the rms linear fluctuation on scales of $8h^{-1}\Mpc$, and the slope of the fluctuation spectrum, where $h$ is the Hubble constant in units of 100 $\kms \oMpc$. We find $σ_8 = 0.80 \pm 0.15$ and $n \sim -1.5$ for $0.5 \le h \le 0.8$, where we assume that the density spectrum is approximated by a power law on cluster scales: $σ(r) \propto r^{-{3+n\over{2}}}$. Our value of $σ_8$ is independent of the density parameter, $Ω_0$, and thus we can estimate $Ω_0$ by combining $σ_8$ obtained in this study with those from $Ω_0$-dependent analyses to date. We find that $σ_8(Ω_0)$ derived from the cluster abundance such as the temperature function gives $Ω_0 \sim 0.5$ while $σ_8(Ω_0)$ measured from the peculiar velocity field of galaxies gives $Ω_0 \sim 0.2-1$, depending on the technique used to analyze peculiar velocity data. Constraints are also derived for open, spatially flat, and tilted Cold Dark Matter models and for Cold + Hot Dark Matter models.