Quasi-bolometric light curve of SN 2010bh produced by using GROND g′r′i′z′   JH filters (black open circles) in the rest frame. For clarity, the uncertainties in the host-galaxy extinction are not included in the error bars. A single black continuous line represents the best-fit model (see Sect. 5.1). Early and late components of the model are smoothly joined at t₀ + 30 d. SE and other GRB-SNe quasi-bolometric light curves have been plotted as a comparison sample: SN 2003lw (GRB 031203; Malesani et al. 2004), SN 1998bw (GRB 980425; Galama et al. 1998b), SN 2006aj (GRB 060218; Pian et al. 2006), the broad-lined Ic SN 2009bb (Pignata et al. 2011), the type-Ic SN 1994I (Richmond et al. 1996), the type Ibc SN 2008D (XRO 080109; Modjaz et al. 2009; Soderberg et al. 2008), and the type-Ic SN 2002ap (Gal-Yam et al. 2002; Foley et al. 2003; Yoshii et al. 2003).