Observational constraints on the free parameters of an interacting Bose-Einstein gas as a dark-energy model

Abstract

Dark energy is modelled by a Bose-Einstein gas of particles with an attractive interaction. It is coupled to cold dark matter, within a flat universe, for the late-expansion description, producing variations in particle-number densities. The model's parameters, and physical association, are: ${\Omega }_{G0}$, ${\Omega }_{m0}$, the dark-energy rest-mass energy density and the dark-matter term scaling as a mass term, respectively; ${\Omega }_{i0}$, the self-interaction intensity; $x$, the energy exchange rate. Energy conservation relates such parameters. The Hubble equation omits ${\Omega }_{G0}$, but also contains $h$, the present-day expansion rate of the flat Friedman--Lemâitre--Robertson--Walker metric, and ${\Omega }_{b0}$, the baryon energy density, used as a prior. This results in the four effective chosen parameters ${\Omega }_{b0}$, $h$, ${\Omega }_{m0}$, ${\Omega }_{i0}$, fit with the Hubble expansion rate $H(z)$, and data from its value today, near distance, and supernovas. We derive wide $1\sigma$ and $2\sigma$ likelihood regions compatible with definite positive total CDM and IBEG mass terms. Additionally, the best-fit value of parameter $x$ relieves the coincidence problem, and a second potential coincidence problem related to the choice of ${\Omega }_{G0}$.

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Cited by in corpus (1)

• Primordial gravitational waves spectrum in the interacting Bose-Einstein gas model