Evolution of the f_bh = 0 model Lagrangian radii and density profile compared with the evolution of models with f_bh = 10⁻³ (left panel) and f_bh = 5 × 10⁻³ (right panel). In the bottom panels the density profile is plotted at t = (0, 5, 10, 15, 20, 25) Gyr of evolution. The blue dashed curves give the evolution of the stellar distribution Lagrangian radii in the models with BHs, and the bottom panels show the respective stellar density profiles at t = (0, 5, 10) Gyr. Over a time of order 10 Gyr, the evolution of the density profile of stars in the f_bh = 10⁻³ model is not much affected by the presence of the BHs. In the model with f_bh = 5 × 10⁻³ the evolution toward the steady state is faster, and after 10 Gyr the stars have formed a cusp. Vertical lines give the MBH influence radius.