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We discuss the effect of ram pressure on the cold clouds in the centers ofcool-core galaxy clusters, and in particular, how it reduces cloud velocity andsometimes causes an offset between the cold gas and young stars. The velocitiesof the molecular gas in both observations and our simulations fall in the rangeof $100-400$ km/s, much lower than expected if they fall from a few tens of kpcballistically. If the intra-cluster medium (ICM) is at rest, the ram pressureof the ICM only slightly reduces the velocity of the clouds. When we assumethat the clouds are actually "fluffier" because they are co-moving with awarm-hot layer, the velocity becomes smaller. If we also consider the AGN windin the cluster center by adding a wind profile measured from the simulation,the clouds are further slowed down at small radii, and the resulting velocitiesare in general agreement with the observations and simulations. Because rampressure only affects gas but not stars, it can cause a separation between afilament and young stars that formed in the filament as they move through theICM together. This separation has been observed in Perseus and also exists inour simulations. We show that the star-filament offset combined withline-of-sight velocity measurements can help determine the true motion of thecold gas, and thus distinguish between inflows and outflows.

The Effects of Ram Pressure on the Cold Clouds in the Centers of Galaxy Clusters