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Tying Dark Matter to Baryons with Self-interactions
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Self-interacting dark matter (SIDM) models have been proposed to solve the small-scale issues with the collisionless cold dark matter (CDM) paradigm. We derive equilibrium solutions in these SIDM models for the dark matter halo density profile including the gravitational potential of both baryons and dark matter. Self-interactions drive dark matter to be isothermal and this ties the core sizes and shapes of dark matter halos to the spatial distribution of the stars, a radical departure from previous expectations and from CDM predictions. Compared to predictions of SIDM-only simulations, the core sizes are smaller and the core densities are higher, with the largest effects in baryon-dominated galaxies. As an example, we find a core size around 0.5 kpc for dark matter in the Milky Way, more than an order of magnitude smaller than the core size from SIDM-only simulations, which has important implications for indirect searches of SIDM candidates.
Forward citations
Cited by 5 Pith papers
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Cloud-9's gas profile can be fit by both cuspy CDM and cored SIDM halos, but matching cosmological halo concentrations favors SIDM with σ/m ≈ 200 cm²/g at about 3σ tension versus 7σ for CDM.
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In a new SIDM simulation of isolated dwarf halos, nine low-mass halos are core-collapsed, and inner density slope—rather than central density—best tracks collapse onset and matches analytic collapse-time predictions.
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Constraints on dark matter self-interaction from velocity distribution function in isolated halos
N-body simulations and rotation-curve data constrain the dark matter self-interaction cross-section to σ/m ≤ 2.7 cm²/g at 95% C.L. for Milky Way-scale halos.
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Relaxing Constraints on Dark Matter Annihilation Near the Supermassive Black Hole in M87
For a Burkert cored M87 halo, the smooth halo, not the black hole density spike, controls the annihilation signal, so M87 constraints on dark matter annihilation weaken by orders of magnitude.
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