New cosmological constraints on the evolution of dark matter energy density

Abstract

We constrain the evolution of dark matter energy density over time, specifically focusing on deviation from the standard model represented by the equation ${\rho }_m\propto (1+z{)}^{3-\epsilon }$, where $\epsilon$ 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 $\epsilon =-0.0073_{-0.0033}^{+0.0029}$, 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.

11 pages, 1 figures, 2 tables. References added. PRD 111, 103534 .(submitted on 28. Feb. 2025). Comments are still welcome. In particular, if you discover that your research is relevant to our work and your findings are not currently listed in Table II of our manuscript, we would greatly appreciate it if you could contact us. We will gladly include your results in the arXiv version of Table II

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