Jeans Model for the Shapes of Self-interacting Dark Matter Halos

TL;DR

This paper extends the Jeans model to predict the shapes of self-interacting dark matter halos, accounting for nonsphericity and validating with simulations, enabling observational tests of dark matter properties.

Contribution

The authors develop a generalized, computationally efficient nonspherical Jeans model for SIDM halos, incorporating multiple scatterings and halo shape predictions beyond spherical symmetry.

Findings

Model accurately reproduces halo shapes in simulations.

Halo shape differences can distinguish SIDM from collisionless dark matter.

Model is validated against cosmological simulations with baryons.

Abstract

The Jeans model is a semi-analytical approach to modeling self-interacting dark matter (SIDM) that works remarkably well to reproduce the spherically-averaged halo profiles from observations and simulations of relaxed galaxies and galaxy clusters. However, SIDM halos are not spherically symmetric in general since they respond to nonspherical baryon distributions and retain nonsphericity from their initial collapse. In this work, we generalize the Jeans model to describe SIDM density profiles and halo shapes beyond spherical symmetry. Observational tests via halo shapes are especially important for testing SIDM in massive galaxies, $M_{\rm 200} \sim 10^{12} - 10^{13} \; \Msun$, where SIDM and collisionless dark matter halos can have indistinguishable spherically-averaged profiles but distinct halo shapes. We validate our model by comparing to cosmological simulations with baryons for both SIDM with $\sigmam = 1 \cmg$ and collisionless cold dark matter. Our approach differs from previous work in this direction, taking into account the fact that multiple scatterings are required to impact the shape of the halo, as well as being computationally inexpensive to implement. The nonspherical Jeans model can be used in conjunction with halo shape observations (e.g., from gravitational lensing or X-ray data) to directly constrain dark matter self-interactions.