Cosmological parameters constraints from galaxy cluster mass function measurements in combination with other cosmological data

TL;DR

This paper combines galaxy cluster mass function data with recent cosmological observations to refine constraints on neutrino properties and dark energy, demonstrating the power of cluster data in cosmological parameter estimation.

Contribution

It provides updated cosmological parameter constraints by integrating galaxy cluster data with recent CMB, Hubble constant, BAO, and supernova data, including neutrino mass and dark energy parameters.

Findings

Constraints on total neutrino mass are around 0.4 eV.

Effective number of neutrino species is approximately 4.

Cluster data provide constraints on dark energy comparable to supernovae.

Abstract

We present the cosmological parameters constraints obtained from the combination of galaxy cluster mass function measurements (Vikhlinin et al., 2009a,b) with new cosmological data obtained during last three years: updated measurements of cosmic microwave background anisotropy with Wilkinson Microwave Anisotropy Probe (WMAP) observatory, and at smaller angular scales with South Pole Telescope (SPT), new Hubble constant measurements, baryon acoustic oscillations and supernovae Type Ia observations. New constraints on total neutrino mass and effective number of neutrino species are obtained. In models with free number of massive neutrinos the constraints on these parameters are notably less strong, and all considered cosmological data are consistent with non-zero total neutrino mass \Sigma m_\nu \approx 0.4 eV and larger than standard effective number of neutrino species, N_eff \approx 4. These constraints are compared to the results of neutrino oscillations searches at short baselines. The updated dark energy equation of state parameters constraints are presented. We show that taking in account systematic uncertainties, current cluster mass function data provide similarly powerful constraints on dark energy equation of state, as compared to the constraints from supernovae Type Ia observations.