Cool circumgalactic gas of passive galaxies from cosmological inflow

The circumgalactic medium (CGM) of galaxies consists of a multi-phase gas with components at very different temperatures, from 10(4) K to 10(7) K. One of the greatest puzzles about this medium is the presence of a large amount of low-temperature (T similar to 10(4) K) gas around quiescent early-type galaxies (ETGs). Using semi-analytical parametric models, we describe the cool CGM around massive, low-redshift ETGs as the cosmological accretion of gas into their dark matter halos, resulting in an inflow of clouds from the external parts of the halos to the central galaxies. We compare our predictions with the observations of the COS-LRG collaboration. We find that inflow models can successfully reproduce the observed kinematics, the number of absorbers and the column densities of the cool gas. Our MCMC fit returns masses of the cool clouds of about 10(5) M-circle dot and shows that they must evaporate during their journey due to hydrodynamic interactions with the hot gas. We conclude that the cool gas present in the halos of ETGs likely cannot reach the central regions and feed the galaxy star formation, thus explaining why these passive objects are no longer forming stars.