Theoretical rise times and end rise absolute magnitudes using the Arnett (1980, 1982) and Rabinak & Waxman (2011) model compared with the SNe in our sample. The SNe are depicted in the same way as in Fig. 8. The shaded regions represent the parameter space for specific progenitor radii, respectively. The input parameters were varied as follows: 100 R_⊙ ≤ R₀ ≤ 900 R_⊙, 0.1 × 10⁵¹ erg ≤ E ≤ 5 × 10⁵¹ erg and 3 ≤ M ≤ 20 M_⊙. The same rise time fitting algorithm was applied to the model optical light curves as was previously applied to the SN data. Only those objects that have progenitor detections are labelled explicitly.