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.
The Dark Matter at the End of the Galaxy
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abstract
Dark matter density profiles based upon Lambda-CDM cosmology motivate an ansatz velocity distribution function with fewer high velocity particles than the Maxwell-Boltzmann distribution or proposed variants. The high velocity tail of the distribution is determined by the outer slope of the dark matter halo, the large radius behavior of the Galactic dark matter density. N-body simulations of Galactic halos reproduce the high velocity behavior of this ansatz. Predictions for direct detection rates are dramatically affected for models where the threshold scattering velocity is within 30% of the escape velocity.
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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.