Radioactive heating model (Arnett 1982) fit to the bolometric (griz) LC of SN 2016jca. Left: two versions of the model have been fit to the data, one that assumes full trapping of γ-rays (red), and one which allows γ-ray leakage (black). It is seen that the latter model better fits the data. Both models require a nickel mass of M_Ni = 0.22M_⊙, an ejecta mass of M_ej = 5.8M_⊙, and for a peak photospheric velocity of v_ph = 29 700 ± 1500 km s^-1, a kinetic energy of E_K = 5.1 ± 0.8 × 10⁵² erg. Both models assume a grey optical opacity of κ = 0.07 cm² g^-1. In the latter model, we find a γ-ray opacity of κ_γ = 0.034 cm² g^-1. Right: comparison of the optical bolometric LCs of a small sample of GRB-SNe: SN 1998bw (BVRI), SN 2003dh (UBVR), SN 2006aj (BVRI), SN 2010bh (griz) and SN 2012bz (griz).