M_f/M_i as a function of M_i/M_crit, assuming that M_i = M_f + M_BH for all simulations considered from Table 1 (top). M_f/M_i as a function of M_i/M_crit (bottom) using the simulations of Reinoso et al. (2020), Vergara et al. (2021, 2023). We show both the result as it would appear considering the approximation used in Eq. B.1 via the solid line and the result when we employ the initial and final stellar masses obtained from the simulation. In the second case the plot is qualitatively similar but with a steeper decrease due to the escapers. The figure also indicates our polynomial fits to the obtained relations.