Top panels show the Lagrangian radii for the four stellar species during the N-body simulations with BH number fractions: f_bh = 10⁻³ (left panels) and f_bh = 5 × 10⁻³ (right panels). Top tick marks give times after scaling to the Milky Way; we adopted a relaxation time at the Sgr A* influence radius of 25 Gyr (e.g., Merritt 2010). Bottom panels show the density profile of stars and BHs at t = (0, 2.5, 5, 7.5, 10) Gyr; the central density increases with time. Clearly, even after a time of the order of 10 Gyr, the distribution of stars and BHs in our models can be very different from the relaxed multi-mass models that are often used to describe the center of galaxies. The vertical line marks the MBH influence radius.