Fig. 5.
Comparison between models (solid lines) and observations (filled dots) for our SN sample. We show 50 models randomly chosen from the posterior probability distribution. Left: bolometric LC. Right: evolution of the photospheric velocity. From top to bottom: SN 2004A, SN 2004et, SN 2005cs, and SN 2008bk. The grey shaded region shows the early data we removed from the fitting. For SN 2004et we show the results using d = 5.9 ± 0.4 Mpc to calculate the bolometric LC.
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