Stellar remnants accretion rate onto the NSC for 50 GCs models for r_hm=2 pc. Left: the mass-time distribution for stellar remnants (WDs, NSs, and BHs); right: for all stars. From the left graph, the boundary between white dwarfs at the bottom and neutron stars and black holes at the top is clearly visible (compact object mass gap). It is also clearly seen in the right figure that the main accretion number contribution comes from low-mass stars, approximately up to ∼ 1.4 solar masses (according to the Chandrasekhar limit).