Formation of Dark Matter Haloes in a Homogeneous Dark Energy Universe

TL;DR

This paper compares the effectiveness of the Press-Schechter and Power Law mass functions in modeling dark matter haloes within a homogeneous dark energy universe, using observational data to evaluate their fit and implications for dark energy properties.

Contribution

It introduces the use of a nonextensive q-statistical distribution (Power Law mass function) for primordial density fields and demonstrates its superior fit to observational data over the traditional Press-Schechter approach.

Findings

Press-Schechter cannot simultaneously fit X-ray and CMB data.

Power Law mass function provides better data fits and constrains dark energy parameters.

The dark energy equation of state parameter is sensitive to the PL free parameter q.

Abstract

Several independent cosmological tests have shown evidences that the energy density of the Universe is dominated by a dark energy component, which cause the present accelerated expansion. The large scale structure formation can be used to probe dark energy models, and the mass function of dark matter haloes is one of the best statistical tools to perform this study. We present here a statistical analysis of mass functions of galaxies under a homogeneous dark energy model, proposed in the work of Percival (2005), using an observational flux-limited X-ray cluster survey, and CMB data from WMAP. We compare, in our analysis, the standard Press-Schechter (PS) approach (where a Gaussian distribution is used to describe the primordial density fluctuation field of the mass function), and the PL (Power Law) mass function (where we apply a nonextensive q-statistical distribution to the primordial density field). We conclude that the PS mass function cannot explain at the same time the X-ray and the CMB data (even at 99% confidence level), and the PS best fit dark energy equation of state parameter is $\omega=-0.58$, which is distant from the cosmological constant case. The PL mass function provides better fits to the HIFLUGCS X-ray galaxy data and the CMB data; we also note that the $\omega$ parameter is very sensible to modifications in the PL free parameter, $q$, suggesting that the PL mass function could be a powerful tool to constrain dark energy models.