Running cosmological constant with observational tests

Abstract

We investigate the running cosmological constant model with dark energy linearly proportional to the Hubble parameter, $\Lambda =\sigma H+{\Lambda }_0$, in which the $\Lambda$CDM limit is recovered by taking $\sigma =0$. We derive the linear perturbation equations of gravity under the Friedmann-Lemaïtre-Robertson-Walker cosmology, and show the power spectra of the CMB temperature and matter density distribution. By using the Markov chain Monte Carlo method, we fit the model to the current observational data and find that $\sigma H_0/{\Lambda }_0\lesssim 2.63\times 10^{-2}$ and $6.74\times 10^{-2}$ for $\Lambda (t)$ coupled to matter and radiation-matter, respectively, along with constraints on other cosmological parameters.

12 pages, 5 figures, version accepted by PLB

References in corpus (8)

• Dynamics of dark energy
• The Clustering of the SDSS DR7 Main Galaxy Sample I: A 4 per cent Distance Measure at z=0.15
• Cosmologies with Energy Exchange
• Dark Energy and QCD Ghost
• Gluonic vacuum, q-theory, and the cosmological constant
• Observational constraints on late-time Lambda(t) cosmology
• Evolution of density perturbations in decaying vacuum cosmology
• Evolution of density perturbations in decaying vacuum cosmology: The case of non-zero perturbations in the cosmological term

Cited by in corpus (3)

• Constraints on a special running vacuum model
• Observational constraints on running vacuum model
• Matter density perturbation and power spectrum in running vacuum model