Measuring the Density Fluctuation From the Cluster Gas Mass Function

Details Measuring the Density Fluctuation From the Cluster Gas Mass Function Measuring the Density Fluctuation From the Cluster Gas Mass Function

1997-01-27

arxiv.org/abs/astro-ph/9701201v1

Astronomy and Astrophysics

Astrophysics

9 pages, LaTeX (aaspp4), 6 PostScript figures, submitted to ApJ

Scientific paper

10.1086/304805

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 $\sigma_8$, 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 $\sigma_8 = 0.80 \pm 0.15$ 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: $\sigma(r) \propto r^{-{3+n\over{2}}}$. Our value of $\sigma_8$ is independent of the density parameter, $\Omega_0$, and thus we can estimate $\Omega_0$ by combining $\sigma_8$ obtained in this study with those from $\Omega_0$-dependent analyses to date. We find that $\sigma_8(\Omega_0)$ derived from the cluster abundance such as the temperature function gives $\Omega_0 \sim 0.5$ while $\sigma_8(\Omega_0)$ measured from the peculiar velocity field of galaxies gives $\Omega_0 \sim 0.2-1$, 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.

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