Determine the true central dark-matter profiles of galaxy clusters

Determine whether galaxy clusters generally exhibit substantially shallower or core-like central dark-matter profiles, or instead smaller cores consistent with stringent constraints on self-interaction cross sections, thereby resolving the current observational disagreement at cluster scales.

Background

The paper compares cluster observations that favor substantial cores on scales of approximately 10 kpc with other analyses that favor smaller cores and constrain constant self-interaction cross sections to roughly 0.1–0.3 cm²/g. Because these observational results are not mutually consistent, the actual prevalence and size of cluster dark-matter cores remain unresolved.

The benchmark inelastic-dark-matter model predicts a measurable cluster core, primarily through elastic heat transport, while exothermic and endothermic conversion partially cancel. Improved cluster mass-profile measurements are therefore presented as a direct test of the interaction responsible for the galaxy-scale dark-matter deficit.