Including relativistic and primordial Non-Gaussianity contributions in cosmological simulations by modifying the initial condition

TL;DR

This paper introduces a method to incorporate relativistic and primordial non-Gaussianity effects into Newtonian cosmological simulations through initial conditions, enabling more accurate modeling of large-scale structures.

Contribution

The authors develop a novel approach to include relativistic corrections and primordial non-Gaussianity in initial conditions for cosmological simulations, validated against relativistic and perturbative benchmarks.

Findings

Relativistic and PNG effects are most significant at large scales.

The method aligns well with relativistic simulations and perturbative predictions.

Inclusion of these effects enhances the realism of structure formation models.

Abstract

We present a method to implement relativistic corrections to the evolution of dark matter structures in Newtonian simulations of a LCDM universe via the initial conditions. We take the nonlinear correspondence between the Lagrangian (Newtonian) evolution of dark matter inhomogeneities and the synchronous-comoving (relativistic) matter density description, and use it to promote the relativistic constraint as the initial condition for numerical simulations of structure formation. In this case, the incorporation of Primordial non-Gaussianity (PNG) contributions as initial conditions is straightforward. We implement the relativistic,fNL and gNLcontributions as initial conditions for the L-PICOLA code, and compute the power spectrum and bispectrum of the evolved matter field. We focus specifically on the case of largest values of non-Gaussianity allowed at 1-sigma by Planck observations(fNL=-4.2 and gNL=-7000). As a checkup, we show consistency with the one-loop perturbative prescription and with a fully relativistic simulation (GRAMSES) on the adequate scales. Our results confirm that both relativistic and PNG features are most prominent at very large scales and for squeezed triangulations. We discuss future prospects to probe these two contributions in the bispectrum of the matter density distribution