Abstract
In this paper, we implement a test of the standard law for the dark matter density evolution as a function of redshift. For this purpose, only a flat universe and the validity of the FRW metric are assumed. A deformed dark matter density evolution law is considered, given by rho _c(z) propto (1+z)^{3+epsilon }, and constraints on epsilon are obtained by combining the galaxy cluster gas mass fractions with cosmic chronometers measurements. We find that epsilon =0 within 2sigma c.l., in full agreement with other recent analyses.
Highlights
Considering the cosmic coincidence problem [14], the introduction of an interaction term between the dark sectors of the universe has been shown to be an interesting alternative to solve or alleviate the problem, as extensively discussed in [19] and more recently in [20]
In [26], it was shown that a model of dynamical dark energy and interacting DE-DM approaches become indistinguishable at the background and linear perturbation level
We propose and implement another test to probe a possible evolution of the dark matter density law (ρc(z) ∝ (1 + z)3) using cosmic chronometers along with X-ray gas mass fraction data from Mantz et al [38], to complement our previous works [36,37]
Summary
Considering the cosmic coincidence problem [14], the introduction of an interaction term between the dark sectors of the universe has been shown to be an interesting alternative to solve or alleviate the problem, as extensively discussed in [19] and more recently in [20]. In [26], it was shown that a model of dynamical dark energy and interacting DE-DM approaches become indistinguishable at the background and linear perturbation level. As a direct consequence of the interacting DE-DM models, an investigation on possible departures for the evolution of the dark matter density with respect to the usual a−3 scaling was done in [36] by combining Type Ia supernovae (SNe Ia) observations and gas mass fraction (GMF) measurements in galaxy clusters. This data could neither confirm nor rule out
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