Constraints on dark matter self-interaction from galactic core size

TL;DR

This study uses simulations of isolated galactic haloes to constrain dark matter self-interaction cross-section based on core size observations, providing an upper limit of 9.8 cm^2/g at 95% confidence.

Contribution

It introduces a systematic simulation-based method to constrain dark matter self-interaction from galactic core sizes, highlighting model dependence.

Findings

Upper limit on dark matter self-interaction cross-section: 9.8 cm^2/g

Core size is sensitive to the assumed galactic density profile

Significant dependence of bounds on density distribution models

Abstract

Self-interaction of particulate dark matter may help thermalising the central region of the galactic halo and driving core formation. The core radius is expectedly sensitive to the self-interaction strength of dark matter (DM). In this paper we study the feasibility of constraining dark matter self-interaction from the distribution of the core radius in isolated haloes. We perform systematic DM only $N$-body simulations of spherically symmetric isolated galactic haloes in the mass range of $10^{10} $-$10^{15}M_{\odot}$, incorporating the impact of isotropic DM self-interaction. Comparing the simulated profiles with the observational data, we provide a conservative upper limit on the self-interaction cross-section, $ \sigma/m < $ $ 9.8 $ $\ \rm cm^2 /\rm gm $ at $ 95 \% $ confidence level. We report significant dependence of the derived bounds on the galactic density distribution models assumed for the analysis.