Cosmological parameter estimation from weak lensing. The case of $\Omega_m$, $\sigma_8$

TL;DR

This paper discusses methods for estimating cosmological parameters using weak lensing data, focusing on the two-point correlation function of gravitational shear and comparing it with galaxy cluster counts.

Contribution

It introduces a comparison between weak lensing measurements and galaxy cluster counts for cosmological parameter estimation, and describes software tools for modeling mass distribution.

Findings

Weak lensing provides valuable cosmological information.

Comparison shows potential advantages of lensing over cluster counts.

Software tools facilitate analysis of gravitational lensing data.

Abstract

Propagation of light in the universe with structure which amplify and modify the shape of distant galaxies, producing a correlation between nearby and distant density of galaxies, is a phenomena very important in cosmology for determining cosmological parameters as the {\Lambda}CDM. In this paper, we discuss the estimation of the two point correlation function in the gravitational shear produced by the large scale structure. We will compare the result given by gravitational lensing with the use of another alternatives such as a counting galaxy clusters. We also describe some software used in the gravitational lensing study for determining mass distribution models and images formation.