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The central densities of Milky Way-mass galaxies in cold and self-interacting dark matter models

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Constraining velocity-dependent self-interacting dark matter with the Milky Way's dwarf spheroidal galaxies

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Summary: The study investigates the potential signature of self-interacting dark matter (SIDM) based on the observed anticorrelation between central dark matter (DM) densities of bright Milky Way dwarf spheroidal galaxies (dSphs) and their orbital pericentre distances. By analyzing the range of SIDM scattering cross-section per unit mass, the research finds that different dSph models require varying values of sigma/m(chi) to reproduce the observed central DM densities. Larger cross-sections are correlated with lower collision velocities of DM particles within each subhalo's core, leading to a proposed SIDM particle model involving a DM particle with a mass m(chi) = 53.93 +/- 9.81 GeV interacting through a light mediator of mass m(phi) = 6.6 +/- 0.43 MeV. This cross-section-velocity relation explains the diverse DM profiles of MW dSph satellites and matches observational constraints on larger scales.

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