Cluster mass function (cf. Fig. 4) for the simulation with the fiducial SN feedback model compared to the mass function for a simulation where stars with mass up to 100 M_⊙ can explode as core-collapse SNe (see text for details). Allowing more massive stars to explode as SNe implies an earlier onset of SN feedback due to the shorter time spent on the main sequence. Because the simulation with massive SN progenitors only progressed 500 Myr, we limit the results to clusters formed between 300 and 500 Myr. Note that the earlier onset of SNe results in a mass function without an obvious plateau at lower masses.