Observational constraints on the interacting Ricci dark energy model

Details Observational constraints on the interacting Ricci dark energy model Observational constraints on the interacting Ricci dark energy model

2009-11-25

arxiv.org/abs/0911.4810v2

Phys.Rev.D81:023519,2010

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

11 pages, 3 figures, final version

Scientific paper

10.1103/PhysRevD.81.023519

We consider an extension of the holographic Ricci dark energy model by introducing an interaction between dark energy and matter. In this model, the dark energy density is given by $rho_{Lambda}=-frac{1}{2}alpha M_{p}^{2}{R}$, where ${R}$ is the Ricci scalar curvature, $M_{p}$ is the reduced Planck mass, and $alpha$ is a dimensionless parameter. The interaction rate is given by $Q=gamma H rho_{Lambda}$, where $H$ is the Hubble expansion rate, and $gamma$ is a dimensionless parameter. We investigate current observational constraints on this model by applying the type Ia supernovae, the baryon acoustic oscillation and the CMB anisotropy data. It is shown that a nonvanishing interaction rate is favored by the observations. The best fit values are $alpha=0.45 pm 0.03$ and $gamma=0.15 pm 0.03$ for the present dark energy density parameter $Omega_{Lambda 0}=0.73 pm0.03$.

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