Top row: evolution of 50%, 10%, and 1% Lagrangian radii (orange, gray, and black lines) for simulations 500k-A-R2-10, 500k-A-R4-10, and 500k-C-R4-10. The three simulations are representative of different densities and rotation strengths. The vertical lines indicate the time of core collapse. Higher density GCs show an earlier and deeper collapse, whereas low rotating GCs show a weaker signature of collapse. Bottom row: evolution of the mean mass within the same Lagrangian radii of the top panel. The 1% Lagrangian radii mainly contain massive objects, corresponding to BHs (or their progenitors). High-density and strong rotating GCs mass segregate more efficiently, in timescales of a few hundred million years.