How the Self-Interacting Dark Matter Model Explains the Diverse Galactic Rotation Curves

TL;DR

The paper demonstrates that the self-interacting dark matter (SIDM) model can accurately reproduce the diverse rotation curves of spiral galaxies by accounting for thermalization effects and halo properties, offering a compelling alternative to the cold dark matter paradigm.

Contribution

This study shows that SIDM, combined with the CDM halo concentration-mass relation, explains the full diversity of galaxy rotation curves without additional assumptions.

Findings

SIDM creates large cores in dark matter dominated galaxies.

In luminous galaxies, SIDM results in denser, smaller cores.

The model reproduces rotation curves across a wide velocity range.

Abstract

The rotation curves of spiral galaxies exhibit a diversity that has been difficult to understand in the cold dark matter (CDM) paradigm. We show that the self-interacting dark matter (SIDM) model provides excellent fits to the rotation curves of a sample of galaxies with asymptotic velocities in the 25 to 300 km/s range that exemplify the full range of diversity. We only assume the halo concentration-mass relation predicted by the CDM model and a fixed value of the self-interaction cross section.In dark matter dominated galaxies, thermalization due to self-interactions creates large cores and reduces dark matter densities. In contrast, thermalization leads to denser and smaller cores in more luminous galaxies, and naturally explains the flat rotation curves of the highly luminous galaxies. Our results demonstrate that the impact of the baryons on the SIDM halo profile and the scatter from the assembly history of halos as encoded in the concentration-mass relation can explain the diverse rotation curves of spiral galaxies.