The Intracluster Gas Fraction in X-ray Clusters : Constraints on the Clustered Mass Density

Details The Intracluster Gas Fraction in X-ray Clusters : Constraints on the Clustered Mass Density The Intracluster Gas Fraction in X-ray Clusters : Constraints on the Clustered Mass Density

1997-01-21

arxiv.org/abs/astro-ph/9701148v1

Mon.Not.Roy.Astron.Soc. 292 (1997) 289

Astronomy and Astrophysics

Astrophysics

8 pages, MN style, 2 epfs figures included. Submitted to MNRAS

Scientific paper

The mean intracluster gas fraction of X-ray clusters within their hydrostatic regions is derived from recent observational compilations of David, Jones & Forman and White & Fabian. At radii encompassing a mean density 500 times the critical value, the individual sample bi-weight means are moderately ($2.4 \sigma$) discrepant; revising binding masses with a virial relation calibrated by numerical simulations removes the discrepancy and results in a combined sample mean and standard error $\fbargas(r_{500}) = (0.060 \pm 0.003) \h^{-3/2}$. For hierarchical clustering models with an extreme physical assumption to maximize cluster gas content, this value constrains the universal ratio of total, clustered to baryonic mass $\Omega_m/\Omega_b \le 23.1 \h^{3/2}$; combining with the primordial nucleosynthesis upper limit on $\Omega_b$ results in $\Omega_m \h^{1/2} < 0.60$. A less conservative, physically plausible approach based on low D/H inferences from quasar absorption spectra and accounting for baryons within cluster galaxies yields an estimate $\Omega_m \h^{2/3} = 0.28 \pm 0.07$ with sources of systematic error involved in the derivation providing approximately $35%$ uncertainty. Additional effects which could provide consistency with the Einstein-deSitter case $\Omega_m \se 1$ are presented, and their observable signatures discussed.

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