2015/05/31 by Andrew Robertson, Richard Massey, R. Massey +4 · 1 citation
Physics and Astronomy · #Astrophysics #COSMIC cancer database #Cold dark matter #Computational physics #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Matter power spectrum #Physics #Quantum mechanics #Redshift #Scattering #Universe #astro-ph.CO
paper · pdf · doi:10.1093/mnras/stv1805
v2 matches accepted MNRAS version
openalex publication_date 2015/08/31 · arxiv created 2017/01/16 · arxiv updated 2017/01/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We estimate the rate of dark matter scattering in collapsed structures throughout the history of the Universe. If the scattering cross-section is velocity independent, then the canonical picture is correct that scatterings occur mainly at late times. The scattering rate peaks slightly at redshift z ∼ 6, and remains significant today. Half the scatterings occur after z ∼ 1, in structures more massive than 1012 M⊙. Within a factor of 2, these numbers are robust to changes in the assumed astrophysics, and the scatterings would be captured in cosmological simulations. However, for particle physics models with a velocity-dependent cross-section (as for Yukawa potential interactions via a massive mediator), the scattering rate peaks before z ∼ 20, in objects with mass ≲104 M⊙. These precise values are sensitive to the redshift-dependent mass–concentration relation and the small-scale cut-off in the matter power spectrum. In extreme cases, the qualitative effect of early interactions may be reminiscent of warm dark matter and strongly affect the subsequent growth of structure. However, these scatterings are being missed in existing cosmological simulations with limited mass resolution.