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The decaying vacuum model (DV), treating dark energy as a varying vacuum, hasbeen studied well recently. The vacuum energy decays linearly with the Hubbleparameter in the late-times, $\rho_\Lambda(t) \propto H(t)$, and produces theadditional matter component. We constrain the parameters of the DV model usingthe recent data-sets from supernovae, gamma-ray bursts, baryon acousticoscillations, CMB, the Hubble rate and x-rays in galaxy clusters. It is foundthat the best fit of matter density contrast $\Omega_m$ in the DV model is muchlager 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 normalizedlikelihoods of $\Omega_m$ and $h$ are presented, respectively. %

Observational constraints on decaying vacuum dark energy model