Modelling the environmental dependence of the growth rate

TL;DR

This paper introduces a novel method to analyze the growth rate of cosmic structures based on local density variations, using simulations and a log-normal model, offering new insights for cosmological studies.

Contribution

The paper presents a new approach to model the environmental dependence of the growth rate of cosmic structures using f(Delta) and a log-normal Monte Carlo method, advancing cosmological analysis techniques.

Findings

Structure grows faster in high-density regions.

f(Delta) can be effectively modeled with a log-normal Monte Carlo approach.

Potential for applying this method to galaxy survey data.

Abstract

The growth rate of cosmic structure is a powerful cosmological probe for extracting information on the gravitational interactions and dark energy. In the late time Universe, the growth rate becomes non-linear and is usually probed by measuring the two point statistics of galaxy clustering in redshift space up to a limited scale, retaining the constraint on the linear growth rate f. In this letter, we present an alternative method to analyse the growth of structure in terms of local densities, i.e. f(Delta). Using N-body simulations, we measure the function of f(Delta) and show that structure grows faster in high density regions and slower in low density regions. We demonstrate that f(Delta) can be modelled using a log-normal Monte Carlo Random Walk approach, which provides a means to extract cosmological information from f(Delta). We discuss prospects for applying this approach to galaxy surveys.