BHMF shift, after stellar feedback expels 99% of the gas, for a gaseous stellar cluster as in Figure 3. In the legend we depict the power exponent, α, of several fits, namely of the BH IMF and of the shifted BHMF for several ranges; the whole range of values, the low-mass range up to the initial PISN cutoff, the range within the upper BH mass gap, and if applicable the tail of heavy BHs.