Astrophysical probes of inelastic dark matter with a light mediator

TL;DR

This paper investigates an inelastic dark matter model with a light mediator, calculating self-interaction cross sections and deriving astrophysical constraints to address small-scale structure issues.

Contribution

It introduces a numerical method for precise cross section calculations and maps parameter space where dark matter self-interactions solve small-scale problems.

Findings

Elastic cross section within 1-5 cm^2/g for certain masses

Constraints on mass splitting to prevent halo core collapse

Astrophysical observations can test large self-interaction models

Abstract

We consider an inelastic dark matter model, where a fermion is charged under a broken U(1) gauge symmetry, and introduce a tiny Majorana mass term to split the fermion into two states with the light one being a dark matter candidate. If the gauge boson is light, it can mediate both elastic and inelastic dark matter self-interactions in dark halos, leading to observational consequences. Using a numerical technique based on partial wave analysis, we accurately calculate the elastic and inelastic self-scattering cross sections. We assume a thermal freeze-out scenario and fix the gauge coupling constant using the relic density constraint. Then, we focus on six benchmark masses of dark matter, covering a wide range from $10~{\rm MeV}$ to $160~{\rm GeV}$ and map parameter regions where the elastic scattering cross section per unit mass is within $1~{\rm cm^2/g} - 5~{\rm cm^2/g}$, favored to solve small-scale issues of cold dark matter. If the heavy state can decay to the light state and a massless species, the inelastic up-scattering process can cool the halo and lead to core collapse. Taking galaxies with evidence of dark matter density cores, we further derive constraints on the parameter space. For dark matter masses below $10~{\rm GeV}$, the mass splitting must be large enough to forbid up scattering in the dwarf halo for evading the core-collapse constraint; while for higher masses, the up-scattering process can still be allowed. Our results show astrophysical observations can provide powerful tests for dark matter models with large elastic and inelastic self-interactions.