Lefthand panel: ⁵⁶Ni mass cumulative distributions for SNe Ib, Ic, and Ic-BL observed at peak. The comparison reveals higher ⁵⁶Ni masses for SNe Ic-BL (host extinction included). Shaded areas indicate the uncertainties for each SN, caused by the error on the explosion day. Central panel: ejecta mass (M) cumulative distributions for SNe Ib, Ic, and Ic-BL. SNe Ic and Ic-BL appear more massive than SNe Ib, but the uncertainties are large. Righthand panel: explosion energy (E_K) cumulative distributions for SNe Ib, Ic, and Ic-BL. SNe Ic-BL are clearly more energetic. We compare our results to those of Cano (2013) and Drout et al. (2011) in Sect. 4.1.