A low Hubble Constant from galaxy distribution observations

Abstract

An accurate determination of the Hubble constant remains a puzzle in observational cosmology. The possibility of a new physics has emerged with a significant tension between the current expansion rate of our Universe measured from the cosmic microwave background by the Planck satellite and from local methods. In this paper, new tight estimates on this parameter are obtained by considering two data sets from galaxy distribution observations: galaxy cluster gas mass fractions and baryon acoustic oscillation measurements. Priors from the Big Bang nucleosynthesis (BBN) were also considered. By considering the flat $\Lambda$CDM and XCDM models, and the non-flat $\Lambda$CDM model, our main results are: $H_0=65.9_{-1.5}^{+1.5}$ km s${}^{-1}$ Mpc${}^{-1}$, $H_0=65.9_{-4.0}^{+4.4}$ km s${}^{-1}$ Mpc${}^{-1}$ and $H_0=64.3_{-4.4}^{+4.5}$ km s${}^{-1}$ Mpc${}^{-1}$ in $2\sigma$ c.l., respectively. These estimates are in full agreement with the Planck satellite results. Our analyses in these cosmological scenarios also support a negative value for the deceleration parameter at least in 3$\sigma$ c.l..

16 pages, 6 figues, 2 table, version accepted in JCAP

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• Testing a varying-$\Lambda$ model for dark energy within Co-varying Physical Couplings framework
• Observational constraints on varying fundamental constants in a minimal CPC model
• Probing the dark matter density evolution law with large scale structures
• The Hubble constant from galaxy cluster scaling-relation and SNe Ia observations: a consistency test
• Non-Parametric Analysis for the Dark Matter Density Evolution
• Constraining hydrostatic mass bias and cosmological parameters with the gas mass fraction in galaxy clusters