The Observed Growth of Massive Galaxy Clusters IV: Robust Constraints on Neutrino Properties

TL;DR

This study uses galaxy cluster data combined with other cosmological observations to place robust constraints on neutrino properties, including mass and number of species, within various cosmological models.

Contribution

It provides the first comprehensive constraints on neutrino mass and N_eff using galaxy cluster growth data combined with multiple cosmological probes.

Findings

Neutrino mass sum M_nu < 0.33 eV at 95.4% confidence

Effective number of neutrino species N_eff = 3.4 -0.5 +0.6

Constraints remain robust even when allowing for curvature and tensor modes

Abstract

This is the fourth of a series of papers in which we derive simultaneous constraints on cosmological parameters and X-ray scaling relations using observations of the growth of massive, X-ray flux-selected galaxy clusters. Here we examine the constraints on neutrino properties that are enabled by the precise and robust constraint on the amplitude of the matter power spectrum at low redshift that is available from our data. In combination with cluster gas-mass fraction, cosmic microwave background, supernova and baryon acoustic oscillation data, and incorporating conservative allowances for systematic uncertainties, we limit the species-summed neutrino mass, M_nu, to <0.33 eV at 95.4 per cent confidence in a spatially flat, cosmological constant (LambdaCDM) model. In a flat LambdaCDM model where the effective number of neutrino species, N_eff, is allowed to vary, we find N_eff = 3.4 -0.5 +0.6 (68.3 per cent confidence, incorporating a direct constraint on the Hubble parameter from Cepheid and supernova data). We also obtain results with additional degrees of freedom in the cosmological model, in the form of global spatial curvature (Omega_k) and a primordial spectrum of tensor perturbations (r and n_t). The results are not immune to these generalizations; however, in the most general case we consider, in which M_nu, N_eff, curvature and tensors are all free, we still obtain M_nu < 0.70 eV and N_eff = 3.7 +- 0.7 (at respectively the same confidence levels as above). These results agree well with recent work using independent data, and highlight the importance of measuring cosmic structure and expansion at low as well as high redshifts. Although our cluster data extend to redshift z=0.5, the effect of neutrino mass on the growth of structure at late times is not yet detected at a significant level.