The Effects Of Relativistic Hidden Sector Particles on the Matter Power Spectrum

TL;DR

This paper investigates how relativistic pressure of hidden sector particles influences the matter power spectrum during an early matter-dominated era, affecting microhalo formation and dark matter annihilation signals.

Contribution

It provides a detailed analysis of the suppression of matter perturbations due to relativistic pressure and supplies transfer functions for accurate power spectrum calculations in hidden sector scenarios.

Findings

Relativistic pressure suppresses small-scale perturbations.

Transfer functions enable quick power spectrum computations.

Certain models significantly enhance microhalo abundance.

Abstract

If dark matter resides in a hidden sector minimally coupled to the Standard Model, another particle within the hidden sector might dominate the energy density of the early universe temporarily, causing an early matter-dominated era (EMDE). During an EMDE, matter perturbations grow more rapidly than they would in a period of radiation domination, which leads to the formation of microhalos much earlier than they would form in standard cosmological scenarios. These microhalos boost the dark matter annihilation signal, but this boost is highly sensitive to the small-scale cut-off in the matter power spectrum. If the dark matter is sufficiently cold, this cut-off is set by the relativistic pressure of the particle that dominates the hidden sector. We determine the evolution of dark matter density perturbations in this scenario, obtaining the power spectrum at the end of the EMDE. We analyze the suppression of perturbations due to the relativistic pressure of the dominant hidden sector particle and express the cut-off scale and peak scale for which the matter power spectrum is maximized in terms of the properties of this particle. We also supply transfer functions to relate the matter power spectrum with a small-scale cut-off resulting from the pressure of the dominant hidden sector particle to the matter power spectrum that results from a cold hidden sector. These transfer functions facilitate the quick computation of accurate matter power spectra in EMDE scenarios with initially hot hidden sectors and allow us to identify which models significantly enhance the microhalo abundance.