Dynamical dark energy after Planck CMB final release and H0 tension

Abstract

In this article we compare a variety of well-known dynamical dark energy models using the cosmic microwave background measurements from the 2018 Planck legacy and 2015 Planck data releases, the baryon acoustic oscillations measurements and the local measurements of H0 obtained by the SH0ES (Supernovae, H0, for the Equation of State of Dark energy) collaboration analysing the Hubble Space Telescope data. We discuss the alleviation of H0 tension, that is obtained at the price of a phantom-like dark energy equation of state. We perform a Bayesian evidence analysis to quantify the improvement of the fit, finding that all the dark energy models considered in this work are preferred against the ΛCDM scenario. Finally, among all the possibilities analysed, the CPL model is the best one in fitting the data and solving the H0 tension at the same time. However, unfortunately, this dynamical dark energy solution is not supported by the baryon acoustic oscillations (BAO) data, and the tension is restored when BAO data are included for all the models.

Elucidating cosmological model dependence with $$H_0$$

“…See Table 4 for explicit expressions for the corresponding equations of state w(z) and dark energy densities X (z) := ρ de (z)/ρ de,0 = exp 3 z 0 1+w(z ) 1+z dz . As observed recently in [127], focusing on any particular DDE parametrisation risks biasing the search for DDE, so here we analyse a broad class of models (see also [128]). We will see that our conclusions are robust to the parametrisation.…”

Late Time Attractors of Some Varying Chaplygin Gas Cosmological Models

“…Table 7. Constraints on the model parameters for the interacting varying Chaplygin gas, Equation ( 9), with non-gravitational interaction term Q given by Equation (29). E.5.2 describes the state of the universe where the varying Chaplygin gas, Equation ( 9), is a phantom dark energy.…”

“…Recently another one known as the H 0 tension problem has been added to this list [15][16][17][18]. The goal of this paper is (1) to consider various new cosmological models explaining the late time accelerated expansion of the universe [19][20][21][22][23][24][25][26], and (2) to see whether or not the models solve the H 0 tension problem [27][28][29][30][31][32][33][34][35][36][37]. The analysis of the models is based on two approaches.…”

“…Critical points corresponding to interacting varying Chaplygin gas, Equation(8), for the non-gravitational interaction Q given by Equation(29). Phase space portraits for interacting varying Chaplygin gas, Equation(8).…”

“…The left plot represents the model where the non-gravitational interaction Q is given by Equation(26). The right plot represents the model where the non-gravitational interaction Q is given by Equation(29).…”