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Stellar and Total Baryon Mass Fractions in Groups and Clusters Since Redshift 1

We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a large sample of groups is considered. To this purpose, 91 candidate X-ray groups/poor clusters at redshift 0.1 <= z <= 1 are selected from the COSMOS 2 deg2 survey, based only on their X-ray luminosity and extent. This sample is complemented by 27 nearby clusters with a robust, analogous determination of the total and stellar mass inside R 500. The total sample of 118 groups and clusters with z <= 1 spans a range in M 500 of ~1013-1015 M sun. We find that the stellar mass fraction associated with galaxies at R 500 decreases with increasing total mass as M -0.37 ± 0.04 500, independent of redshift. Estimating the total gas mass fraction from a recently derived, high-quality scaling relation, the total baryon mass fraction (f stars+gas 500 = f stars 500 + f gas 500) is found to increase by ~25%, when M 500 increases from langMrang = 5 × 1013 M sun to langMrang = 7 × 1014 M sun. After consideration of a plausible contribution due to intracluster light (11%-22% of the total stellar mass) and gas depletion through the hierarchical assembly process (10% of the gas mass), the estimated values of the total baryon mass fraction are still lower than the latest CMB measure of the same quantity (WMAP5), at a significance level of 3.3σ for groups of langMrang = 5 × 1013 M sun. The discrepancy decreases toward higher total masses, such that it is 1σ at langMrang = 7 × 1014 M sun. We discuss this result in terms of nongravitational processes such as feedback and filamentary heating.

cosmological parameters; cosmology: observations; diffuse radiation; galaxies: clusters: general; galaxies: stellar content; X-rays: galaxies: clusters

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