2017/05/31 by Thejs Brinckmann, Jesús Zavala, David Rapetti +2
Physics and Astronomy · #Astronomy #Astrophysics #Baryon #Cluster (spacecraft) #Cold dark matter #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Physics #RADIUS #Sigma #Virial mass #Virial theorem #astro-ph.CO
paper · pdf · doi:10.1093/mnras/stx2782
15 pages, 15 figures. Submitted to MNRAS. Revisions: added new figure with an observational comparison of density profiles, improvements and corrections to the section on velocity anisotropies
openalex created_date 2017/05/12 · arxiv created 2017/10/19 · openalex publication_date 2017/10/27 · arxiv updated 2017/12/20 · openalex updated_date 2026/08/05
We perform dark-matter-only simulations of 28 relaxed massive cluster-sized haloes for cold dark matter (CDM) and self-interacting dark matter (SIDM) models, to study structural differences between the models at large radii, where the impact of baryonic physics is expected to be very limited. We find that the distributions for the radial profiles of the density, ellipsoidal axial ratios and velocity anisotropies (β) of the haloes differ considerably between the models (at the ∼1σ level), even at ≳ 10 per cent of the virial radius, if the self-scattering cross-section is σ/mχ = 1 cm2 g−1. Direct comparison with observationally inferred density profiles disfavours SIDM for σ/mχ = 1 cm2 g−1, but in an intermediate radial range ( ∼ 3 per cent of the virial radius), where the impact of baryonic physics is uncertain. At this level of the cross-section, we find a narrower β distribution in SIDM, clearly skewed towards isotropic orbits, with no SIDM (90 per cent of CDM) haloes having β > 0.12 at 7 per cent of the virial radius. We estimate that with an observational sample of ∼30 (∼1015 M⊙) relaxed clusters, β can potentially be used to put competitive constraints on SIDM, once observational uncertainties improve by a factor of a few. We study the suppression of the memory of halo assembly history in SIDM clusters. For σ/mχ = 1 cm2 g−1, we find that this happens only in the central halo regions (∼1/4 of the scale radius of the halo), and only for haloes that assembled their mass within this region earlier than a formation redshift zf ∼ 2. Otherwise, the memory of assembly remains and is reflected in ways similar to CDM, albeit with weaker trends.