Mass fraction formed in δt = 10 Myr in stars less massive than 0.5 M_⊙ relative to the total initial mass in the IGIMF models (Eq. (12)) is shown in dependence of the SFR and [Fe/H]. The canonical IMF is depicted as the horizontal black line (F₀₅ ≈ 0.25). We note that the IGIMF1 and IGIMF2 models lead to F05 values as if the gwIMF were bottom heavy in comparison with the canonical IMF. However this is due to the normalization caused by the IGIMF being top light for low SFRs (<1 M_⊙ yr⁻¹).