Dianoga SIDM: galaxy cluster self-interacting dark matter simulations
arxiv(2024)
Abstract
This work aims at assessing the impact of DM self-interactions on the
properties of galaxy clusters. In particular, the goal is to study the angular
dependence of the cross section by testing rare (large angle scattering) and
frequent (small angle scattering) SIDM models with velocity-dependent cross
sections. We re-simulate six galaxy cluster zoom-in initial conditions with a
dark matter only run and with a full-physics setup simulations that includes a
self-consistent treatment of baryon physics. We test the dark matter only setup
and the full physics setup with either collisionless cold dark matter, rare
self-interacting dark matter, and frequent self-interacting dark matter models.
We then study their matter density profiles as well as their subhalo
population. Our dark matter only SIDM simlations agree with theoretical models,
and when baryons are included in simulations, our SIDM models substantially
increase the central density of galaxy cluster cores compared to full-physics
simulations using collisionless dark matter. SIDM subhalo suppression in
full-physics simulations is milder compared to the one found in dark matter
only simulations, because of the cuspier baryionic potential that prevent
subhalo disruption. Moreover SIDM with small-angle scattering significantly
suppress a larger number of subhaloes compared to large angle scattering SIDM
models. Additionally, SIDM models generate a broader range of subhalo
concentration values, including a tail of more diffuse subhaloes in the
outskirts of galaxy clusters and a population of more compact subhaloes in the
cluster cores.
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