Constraints on shear and rotation with massive galaxy clusters

Abstract

A precise determination of the mass function is an important tool to verify cosmological predictions of the $\Lambda$CDM model and to infer more precisely the better model describing the evolution of the Universe. Galaxy clusters have been currently used to infer cosmological parameters, in particular the matter density parameter ${\Omega }_{\mathrm{m}}$, the matter power spectrum normalization ${\sigma }_8$ and the equation of state parameter $w_{\mathrm{de}}$ of the dark energy fluid. In this work, using data on massive galaxy clusters ($M>8\times 10^{14}{h}^{-1}{M}_{\odot }$) in the redshift range $0.05\lesssim z\lesssim 0.83$ we put constraints on the parameter $\alpha$ introduced within the formalism of the extended spherical collapse model to quantify deviations from sphericity due to shear and rotation. Since at the moment there is no physical model describing its functional shape, we assume it to be a logarithmic function of the cluster mass. By holding ${\sigma }_8$ fixed and restricting our analysis to a $\Lambda$CDM model, we find, at $1-\sigma$ confidence level, ${\Omega }_{\mathrm{m}}=0.284\pm 0.0064$, $h=0.678\pm 0.017$ and $\beta =0.0019_{-0.0015}^{+0.0008}$, where $\beta$ represents the slope of the parameter $\alpha$. This results translates into a $9\%$ decrement of the number of massive clusters with respect to a standard $\Lambda$CDM mass function, but better data are required to better constrain this quantity, since at the $2-\sigma$ and $3-\sigma$ confidence level we are only able to infer upper limits.

Accepted for publication in MNRAS

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• Improved Lemaitre-Tolman model and the mass and turn-around radius in group of galaxies