Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component

Abstract

We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 10 10 ) < 0.21 is hold.

Modified holographic Ricci dark energy coupled to interacting relativistic and non-relativistic dark matter in the nonflat universe

“…Using the χ 2 method to the observational Hubble data, Chimento et al . find it is consistent with the bound Ω de (z ≃ 1100) < 0.1 reported for the behavior of DE at an early stage [91], and more of their work about the interacting modified holographic Ricci dark energy (IMHRDE) model can be found in [97,98]. The MHRDE interacting with pressureless non-relativistic DM in a flat Friedmann-Robertson-Walker (FRW) universe has been studied by Chattopadhyay et al .…”

Scalar perturbations in cosmological models with dark energy-dark matter interaction

“…As an example of such a coupling, let us mention the mass of CDM particles depending on the dark energy field [9]. It should be mentioned in addition that the introduction of dark sector interactions is also reasonable for the holographic scenario [10,11]. Besides, the data of observations from the Abell Cluster A586 [12][13][14], measurements of the baryon acoustic oscillations of the Lyman alpha forest from high redshift quasars [15] as well as the cosmic microwave background and redshift-space distortions measurements [16] may indicate the reality of these interactions.…”

On extended sign-changeable interactions in the dark sector

“…This best fit value for the transition redshift z acc = 0.805 is significantly higher than that obtained in [73] at 1σ CL analyzing distinct databases and in a model-independent way. However, it is typical for models with interactions in the dark sector [57,[74][75][76][77][78].…”