Ponente
Descripción
We compare the statistics and morphology of arcs in galaxy clusters using simulations with standard cold dark matter and simulations where dark matter has a probability of interaction (parametrized by its cross section), i.e self-interacting dark matter. Through ray tracing, we produce a statistically large number of arcs around galaxy clusters at different redshifts. Since dark matter in more likely to interact in colliding clusters than in relaxed clusters, and this probability of interaction is largest in the denser regions, we focus our analysis on radial arcs (which trace the lensing potential in the central region better than tangential arcs), in galaxy clusters which are undergoing a major merger. We find that self-interacting dark matter produces fewer radial arcs than standard cold dark matter but they are on average more magnified. We also appreciate differences in the morphology which could be used to statistically favor one model versus the other.
