Range of parameters in which the proto-BHMF-shift operates. The rows correspond to different stellar-cluster total masses and the columns to different metallicities. The solid shaded blue region in the ε-r_h plane signifies their range in which the most massive BH grows by at least 10 M_⊙. The diagonally hatched region signifies additionally the ε-r_h range for which an IMBH with a mass of ~10³ M_⊙ can be generated. Notice that the subsolar and low-metallicity cases require an almost identical cluster compactness for the BHMF-shift to operate, but the solar metallicity case requires about double or higher compactness (x axis).