Epochs of maximum light and bolometric light curves of type Ia supernovae

We present empirical fits to the UBVRI light curves of type Ia supernovae. These fits an used to objectively evaluate tight curve parameters. We find that the relative times of maximum light in the filter passbands are very similar for most objects. Surprisingly the maximum at longer wavelengths is reached earlier than in the B and V light curves. This clearly demonstrates the complicated nature of the supernova emission. Bolometric light curves for a small sample of well-observed SNe Ia are constructed by integration over the optical filters. In most objects a plateau or inflection is observed in the light curve about 20-40 days after bolometric maximum. The strength of this plateau varies considerably among the individual objects in the sample. Furthermore the rise times show a range of several days for the few objects which have observations early enough for such an analysis. On the other hand, the decline rate between 50 and 80 days past maximum is remarkably similar for all objects, with the notable exception of SN 1991bg. The similar late decline rates for the supernovae indicate that the energy release at late times are very uniform; the differences at early times an likely due to the radiation diffusing out of the ejecta. With the exception of SN 1991bg, the range of absolute bolometric luminosities of SNe Ia is found to be at least a factor of 2.5. The nickel masses derived from this estimate range from 0.4 to 1.1 M-circle dot. It seems impossible to explain such a mass range by a single explosion mechanism, especially since the rate of gamma-ray escape at late phases seems to be very uniform.