Bolometric light curves of SE-SNe. SN 2011kl is seen to exceed all other well-monitored GRB-SNe (Olivares et al. 2012, 2015; Prentice et al. 2016) in luminosity, including the bright GRB 120422A/SN 2012bz (Schulze et al. 2014) and the recent well-monitored GRB 130702A/SN 2013dx (Toy et al. 2016). SN 2011kl is far less luminous than SLSNe, exemplified in this figure by PTF12dam (Chen et al. 2015), but of similar luminosity as one of the rapidly rising gap transients (RRGTs) presented by Arcavi et al. (2016); the light-curve evolution is also similar. We assign SNLS06D1hc the same peak time as SN 2011kl. Several further luminous SNe are also shown (see Sect. 4.1.4 for more details). Additionally, we plot mean light curves of four different SE-SNe types taken from Lyman et al. (2016) as well as SN 1987A, which had a BSG progenitor (Suntzeff & Bouchet 1990). We assume t_peak = 64 days for PTF12dam (Nicholl et al. 2013; Chen et al. 2015) and t_peak = 19 days for the average curves (Lyman et al. 2016).