Cosmological perturbations in the $\Lambda$CDM-like limit of a polytropic dark matter model

TL;DR

This paper investigates cosmological perturbations within a polytropic dark matter model that mimics $ m extLambda$CDM, showing it aligns well with structure formation observations and reproduces key features like the scalar spectral index.

Contribution

It demonstrates that the $ m extLambda$CDM-like limit of a polytropic dark matter model accurately reproduces structure formation effects and the observed scalar spectral index.

Findings

Reproduces key effects of standard structure formation theory.

Scalar spectral index matches Planck observations ($n_s=0.970$).

Small-scale velocity perturbations slightly increase over time.

Abstract

In a recent article, Kleidis and Spyrou (2015) proposed that both dark matter (DM) and dark energy (DE) can be treated as a single component, if accommodated in the context of a polytropic DM fluid with thermodynamical content. Depending only on the polytropic exponent, $-0.103 < \Gamma \leq 0$, this unified DM model reproduces to high accuracy the distance measurements performed with the aid of the supernovae Type Ia (SNe Ia) standard candles, without suffering either from the age or from the coincidence problem. To demonstrate also its compatibility with current observational data concerning structure formation, in the present article we discuss the evolution of cosmological perturbations in the $\Lambda$ CDM-like (i.e., $\Gamma = 0$) limit of the polytropic DM model. The corresponding results are quite encouraging, since, such a model reproduces every major effect already known from conventional (i.e., pressureless cold dark matter - CDM) structure formation theory, such as the constancy of metric perturbations in the vicinity of recombination and the (late-time) Meszaros effect on their rest-mass density counterparts (Meszaros 1974). The non-zero (polytropic) pressure, on the other hand, drives the evolution of small-scale velocity perturbations along the lines of the root-mean-square velocity law of conventional Statistical Physics. As a consequence, in this model "peculiar velocities" slightly increase, instead of being redshifted away by cosmic expansion. What is more important is that, upon consideration of scale-invariant metric perturbations, the spectrum of their rest-mass density counterparts exhibits an effective power-law dependence on the (physical) wavenumber, with the associated scalar spectral index being equal to $n_s = 0.970$; a theoretical value that actually reproduces the corresponding observational (Planck) result (Ade et al. 2016).