New cosmological constraints on the evolution of dark matter energy density

TL;DR

This study uses multiple observational datasets to tightly constrain the evolution of dark matter energy density, providing evidence for a slight interaction with dark energy that deviates from the standard non-interacting model.

Contribution

It offers the first comprehensive constraint on the dark matter evolution parameter using diverse datasets including DESI BAO, Planck CMB, cosmic chronometers, SNIa, and RSD measurements.

Findings

The deviation parameter ε is constrained to approximately -0.0073.

Results indicate a ~2.4σ deviation from the non-interacting dark matter model.

Findings support the possibility of interaction between dark matter and dark energy.

Abstract

We constrain the evolution of dark matter energy density over time, specifically focusing on deviation from the standard model represented by the equation $\rho_{m}\propto(1+z)^{3-\varepsilon}$, where $\varepsilon$ is a constant parameter. Utilizing a diverse array of observational datasets, including baryon acoustic oscillations (BAO) data from the first release of the Dark Energy Spectroscopic Instrument (DESI), distance priors derived from cosmic microwave background (CMB) observations by the Planck satellite, Hubble rate data obtained through the cosmic chronometers (CC) method, type Ia supernova (SNIa) data from the Panthon sample, and the data from the redshift space distortion (RSD) measurements ($f\sigma_8$), we derive stringent constraints on the deviation parameter. We find that for the model under consideration, the deviation parameter is constrained to be $\varepsilon = -0.0073^{+0.0029}_{-0.0033}$, indicating a deviation of approximately $2.4\sigma$ from the scenario where dark matter and vacuum dark energy do not interact. When compared with previous studies and alternative analyses, our findings provide corroborative evidence for an interaction between dark matter and vacuum dark energy, particularly in light of the release of BAO data from DESI.