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The interaction of gas-rich galaxies with the intra-cluster medium (ICM) ofgalaxy clusters has a remarkable impact on their evolution, mainly due to thegas loss associated with this process. In this work, we use an idealised,high-resolution simulation of a Virgo-like cluster, run with RAMSES and withdynamics reproducing that of a zoom cosmological simulation, to investigate theinteraction of infalling galaxies with the ICM. We find that the tails of rampressure stripped galaxies give rise to a population of up to more than ahundred clumps of molecular gas lurking in the cluster. The number count ofthose clumps varies a lot over time -- they are preferably generated when alarge galaxy crosses the cluster (M$_{200c} > 10^{12}$ M$_\odot$), and theirlifetime ($\lesssim 300$ Myr) is small compared to the age of the cluster. Wecompute the intracluster luminosity associated with the star formation whichtakes place within those clumps, finding that the stars formed in all of thegalaxy tails combined amount to an irrelevant contribution to the intraclusterlight. Surprisingly, we also find in our simulation that the ICM gassignificantly changes the composition of the gaseous disks of the galaxies:after crossing the cluster once, typically 20% of the cold gas still in thosedisks comes from the ICM.

Free-floating molecular clumps and gas mixing: hydrodynamic aftermaths of the intracluster$-$interstellar medium interaction