Observational constraints on decaying vacuum dark energy model

The decaying vacuum model (DV), treating dark energy as a varying vacuum, has been studied well recently. The vacuum energy decays linearly with the Hubble parameter in the late-times, rho(Lambda)(t) alpha H(t), and produces the additional matter component. We constrain the parameters of the DV model using the recent data-sets from supernovae, gamma-ray bursts, baryon acoustic oscillations, CMB, the Hubble rate and X-rays in galaxy clusters. It is found that the best fit of the matter density contrast Omega(m) in the DV model is much lager than that in Lambda CDM model. We give the confidence contours in the Omega(m)-h plane up to 3 sigma confidence level. Besides, the normalized likelihoods of Omega(m) and h are presented, respectively.