Post-collapse density profile in gas models of two-component systems with M₂/M₁ = 0.01 near the onset of gravothermal oscillations for m₂/m₁ = 50 (N = 4.3 × 10⁶, top) and m₂/m₁ = 10 (N = 8.5 × 10⁵, bottom). The following is shown in the plot: ρ₁ (thin line), ρ₂ (thick line), ρ_tot (dashed line), core radius of heavy component r_c,2 (×), core radius of light component r_c,1 (*) and r_h,2 (+). The core radii have been defined as |$r_{{\rm c},i}=\sqrt{9\sigma _{{\rm c},i}^2/(4\pi \rho _{{\rm c},i})}$|⁠. For the case m₂/m₁ = 50, the BH subsystem creates a density hole in the light component: the density of lights in the centre is approximately a factor of 2 less than its highest value (which occurs at log r/r_h ≃ −0.5). The remarkably large value of r_c,1 for this case results from the low value of ρ_c,1 and a high value of |$\sigma _{\rm c,1}^2$| caused by the presence of the BH subsystem.