The cluster gas mass fraction as a cosmological probe: a revised study

TL;DR

This study uses X-ray observations of galaxy clusters to measure their baryon content and constrain cosmological parameters, highlighting the importance of systematics and the potential for cluster baryon fractions to inform cosmology.

Contribution

It provides a revised analysis of cluster baryon fractions as a cosmological probe, incorporating systematics and using a sample of 52 clusters to constrain Omega, Lambda, and w.

Findings

Omega is constrained to 0.35 with 11% statistical uncertainty.

Constraints on Lambda and w are weaker due to larger uncertainties.

Non-thermal pressure and clumpiness are limited to about 10%.

Abstract

(Abriged) We present the analysis of the baryonic content of 52 X-ray luminous galaxy clusters observed with Chandra in the redshift range 0.3-1.273. We use the deprojected X-ray surface brightness profiles and the measured values of the gas temperature to recover the gas and total mass profiles. By assuming that galaxy clusters are representative of the cosmic baryon budget, the distribution of the cluster baryon fraction in the hottest (T> 4 keV) systems as a function of redshift is used to constrain the cosmological parameters. We discuss how our constraints are affected by several systematics, namely the isothermality, the assumed baryon fraction in stars, the depletion parameter and the sample selection. By using only the cluster baryon fraction as a proxy for the cosmological parameters, we obtain that Omega is very well constrained at the value of 0.35 with a relative statistical uncertainty of 11% (1 sigma level; w=-1) and a further systematic error of about (-6,+7)%. On the other hand, constraints on Lambda (without the prior of flat geometry) and w (using the prior of flat geometry) are definitely weaker due to the presence of larger statistical and systematic uncertainties (of the order of 40 per cent on Lambda and larger than 50 per cent on w). If the WMAP 5-year best-fit results are assumed to fix the cosmological parameters, we limit the contributions expected from non-thermal pressure support and ICM clumpiness to be lower than about 10 per cent, leaving also room to accommodate baryons not accounted for either in the X-ray emitting plasma or in stars of the order of 18 per cent of the total cluster baryon budget.