Speaker
Description
Self-interaction of particulate dark matter may help thermalising the galactic center and driving core formation. The core radius is expectedly sensitive to the self-interaction strength of dark matter. In this work we study the feasibility of constraining dark matter self-interaction from the distribution of core radius in isolated haloes. We perform systematic $N$-body simulations of isolated galactic haloes in the mass range of $10^{10} $-$10^{15}M_{\odot}$, incorporating the impact of dark matter self-interaction, having an interaction strength $\sigma/m $ in the range of $ (0-10) \, \rm cm^{2}/ \rm gm $. With zero scattering cross-section signifying the collision-less cold dark matter scenario. Comparing the simulated dark matter density profiles with the observational data from dwarf galaxies, low surface brightness galaxies and galaxy clusters, we provide a conservative upper limit on the self-interaction cross-section, $ \sigma/m < $ $ 9.8 $ $\ \rm cm^2 /\rm gm $ at $ 95 \% $ confidence. We also report significant dependence of the derived bounds on the galactic density distribution models assumed for the analysis.
| In-person participation | Yes |
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