Simulations of Large-Scale Cold Fronts and Subcluster Interactions in the Perseus Cluster

The Perseus Cluster is a well-studied system in the X-rays, presenting spiral-shaped cold fronts which extend to large radii. These features are believed to be caused by the sloshing motion of the gas after the passage of a subcluster. We present simulations of the formation of sloshing cold fronts in Perseus using the AREPO magnetohydrodynamics code, with the aim of reproducing the positions of the observed fronts. Our simulations explore a range of initial conditions, including different subcluster masses and impact parameters. We will address questions such as what is required to generate and sustain a CF that is capable of propagating to such a large radius. What characteristics does the merger need to have to prevent the disruption of the CF before it reaches distances from the core? Not only we will show how the different parameters affect various aspects of the cold fronts, including the time it takes for the first fronts formed to reach large radii, as well as the number and positions of the fronts, but also place constraints on the possible position and trajectory of the subcluster. This is a separate but important issue since in many sloshing-CF clusters - including Perseus - the identity of the subcluster is not readily apparent and no identifiable structure is visible in the X-ray observations.