The Baryon Fraction and Velocity--Temperature Relation in Galaxy Clusters : Models versus Observations

Details The Baryon Fraction and Velocity--Temperature Relation in Galaxy Clusters : Models versus Observations The Baryon Fraction and Velocity--Temperature Relation in Galaxy Clusters : Models versus Observations

1995-09-28

arxiv.org/abs/astro-ph/9509148v1

Astrophys.J. 460 (1996) 10

Astronomy and Astrophysics

Astrophysics

17 pages, uuencoded, compressed Postscript file, to appear in Astrophysical Journal

Scientific paper

10.1086/176948

The observed baryon fraction and velocity--temperature relation in clusters of galaxies are compared with hydrodynamic simulations in two cosmological models : standard (Omega = 1) and a low-density flat (Omega=0.45 and \lambda=0.55) CDM models, normalized to the COBE background fluctuations. The observed properties of clusters include the velocity dispersion versus temperature relation, the gas mass versus total mass relation, and the gas mass fraction versus velocity dispersion relation. We find that, while both cosmological models reproduce well the shape of these observed functions, only low-density CDM can reproduce the observed amplitudes. The cluster gas mass fraction reflects approximately the baryon fraction in the models, with a slight anti-bias. Therefore, due to the low baryon density given by nucleosynthesis, Omega = 1 models produce too few baryons in clusters compared with observations. Scaling our results as a function of Omega, we find that a low-density CDM model, with Omega approximately 0.3 - 0.4, best reproduces the observed mean baryon fraction in clusters. The observed beta parameter of clusters, beta = sigma^2/(k T/mu m_p) = 0.94 \pm 0.08 discriminates less well between the models; it is consistent with that produced by low-density CDM (1.10 \pm 0.22), while it is slightly larger than expected but still consistent with Omega = 1 (0.70 \pm 0.14).

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