Dependence of the inner dark matter profile on the halo mass

• DOI: 10.1046/j.1365-8711.2003.06910.x
• Publication Date: 2003-09-22T12:54:54Z
• Authors: Massimo Ricotti
• Keywords: Cold dark matter

I compare the density profile of dark matter (DM) halos in cold (CDM) N-body simulations with 1 Mpc, 32 256 Mpc and 1024 box sizes. In dimensionless units differ only for initial power spectrum perturbations. profiles when most massive are composed about 10^5 DM particles. The show systematically shallower cores respect to corresponding simulation that have masses, M_{dm}, typical Milky Way fitted by a NFW profile. consistent having steeper than simulation, but higher mass resolution needed strengthen this result. Combined, these results indicate is not universal, presenting dwarf galaxies clusters. Physically result sustains hypothesis function accreting satellites determines inner slope comoving coordinates, r, ρ_{dm} \propto 1/(X^α(1+X)^{3-α}), X=c_Δr/r_Δ, r_Δis virial radius α=α(M_{dm}), provides good fit all from clusters at any redshift same concentration parameter c_Δ~ 7. slope, γ, outer parts halo appears depend on acceleration universe: scale a=(1+z)^{-1} < 1, γ~ 3 as profile, 4 > Ω_Λ~ universe inflating.[abridged]