http://arxiv.org/abs/1402.2590
Measurements of the cluster abundance as a function of mass and redshift provide an important cosmological test that probe not only the expansion rate but also the growth of perturbations. In this paper we adopt a scalar field scenario which admits both thawing and freezing solutions from an appropriate choice of the model parameters and derived all relevant expressions to calculate the mass function and the cluster number density assuming the well-known Sheth-Torman formalism. We discuss the ability of cluster observations to distinguish between these scalar field behaviours and the standard $\Lambda$CDM scenario by considering the eROSITA and SPT cluster surveys.
N. Devi and J. Alcaniz
Wed, 12 Feb 14
20/67
You must be logged in to post a comment.