Notes. This table summarizes the variations of the stellar IMF resulting in different IGIMFs implemented in this work. The α_i coefficients are defined in Eq. (4). We note that the model IGIMF1 assumes the IMF to be the invariant canonical form and corresponds to the original formulation of the IGIMF theory (Kroupa & Weidner 2003; Weidner & Kroupa 2006) before evidence for the variation of the stellar IMF was quantified, the model IGIMF2 assumes that only the upper end of the IMF varies with density and metallicity, while the model IGIMF3 assumes the IMF varies over all stellar masses.