Remnant production and retention in the NBODY7-computed, M_cl(0) ≈ 5.0 × 10⁴ M_⊙, r_h(0) ≈ 2 pc model cluster with all BH-progenitor stars paired in primordial binaries (see Sect. 4). The legends are the same as in the top panels of Fig. 12. The panels show different computations that adopt different extents of mass loss during a star-star merger process: the left panel shows the case that has defaulted in NBODY7/BSE, namely, mass-loss fraction of f_mrg = 0.3 from the secondary for energetic MS-MS collisions only (see text) and zero otherwise (the data in this panel are identical to those in the top right panel of Fig. 12), the middle panel shows the NBODY7 computation where a mass-loss fraction of f_mrg = 0.5 from the secondary is implemented for all star-star mergers, and the right panel shows the computation where a mass-loss fraction of f_mrg = 0.8 from the secondary is implemented for all star-star mergers. With increasing extent of mass loss in mergers (left to right panel), the single-star ZAMS mass-remnant mass relation (orange, empty squares) gets affected by massive-stellar mergers (black, filled squares) to a diminishing extent. The F12-rapid remnant-formation prescription, including PPSN/PSN, and Z = 0.0001, is assumed in this demonstration.