Papers › Cosmological Constraints from Gas Mass Fractions of Massive, Relaxed Galaxy Clusters
Cosmological Constraints from Gas Mass Fractions of Massive, Relaxed Galaxy Clusters
Adam B. Mantz, Steven W. Allen, Rebecca E. A. Canning, Lucie Baumont, Bradford Benson, Lindsey E. Bleem, Steven R. Ehlert, Benjamin Floyd, Ricardo Herbonnet, Patrick L. Kelly, Shuang Liang, Anja von der Linden, Michael McDonald, David A. Rapetti, Robert W. Schmidt, Norbert Werner, Adam Wright
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We present updated cosmological constraints from measurements of the gas mass fractions (f_(gas)) of massive, dynamically relaxed galaxy clusters. Our new data set has greater leverage on models of dark energy, thanks to the addition of the Perseus Cluster at low redshifts, two new clusters at redshifts z>0.97, and significantly longer observations of four clusters at 0.6<z<0.9. Our low-redshift (z<0.16) f_(gas) data, combined with the cosmic baryon fraction measured from the cosmic microwave background (CMB), imply a Hubble constant of h = 0.722 ±0.067. Combining the full f_(gas) data set with priors on the cosmic baryon density and the Hubble constant, we constrain the dark energy density to be Ω_Λ = 0.865 ±0.119 in non-flat ΛCDM (cosmological constant) models, and its equation of state to be w = -1.13_(-0.20)^(+0.17) in flat, constant-w models, respectively 41 and 29 per cent tighter than our previous work, and comparable to the best constraints available from other probes. Combining f_(gas), CMB, supernova, and baryon acoustic oscillation data, we also constrain models with global curvature and evolving dark energy. For the massive, relaxed clusters employed here, we find the scaling of f_(gas) with mass to be consistent with a constant, with an intrinsic scatter that corresponds to just 3 per cent in distance.
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