Radial profile of the ratio between the density of BHs, ρ_bh, and stellar densities, ρ_st, for simulations A1 (continue curve) and A2 (dot–dashed curve). The dotted curve shows the value corresponding to the initial cluster models before the BHs segregated to the center. The latter is also the density ratio expected in the absence of dynamical evolution. Within 5 pc our models predict larger BH densities than what is expected if the remnant population had the same density distribution of stars at the time the clusters reach their tidal disruption radius. As discussed in the text, where ρ_bh 0.1ρ_st, the evolution of the stars is expected to be dominated by gravitational interaction with the BHs, as opposed to self-interactions.