Signatures of Self-Interacting dark matter on cluster density profile
  and subhalo distributions
  Non-gravitational interactions between dark matter particles with strong
scattering, but relatively small annihilation and dissipation, has been
proposed to match various observables on cluster and group scales. In this
paper, we present the results from large cosmological simulations which include
the effects of different self-interaction scenarios. In particular we explore a
model with the differential cross section that can depend on both the relative
velocity of the interacting particles and the angle of scattering. We focus on
how quantities, such as the stacked density profiles, subhalo counts and the
splashback radius change as a function of different forms of self-interaction.
We find that self-interactions not only affect the central region of the
cluster, the effect well known from previous studies, but also significantly
alter the distribution of subhalos and the density of particles out to the
splashback radius. Our results suggest that current weak lensing data can
already put constraints on the self-interaction cross-section that are only
slightly weaker than the Bullet Cluster constraints ($\sigma/m \lesssim 2$
cm$^2/$g), and future lensing surveys should be able to tighten them even
further making halo profiles on cluster scales a competitive probe for DM
physics.
