The model of supernova

To model the lightcurves, we need to know the brightness of the supernovæ of the Ia type according to time and wavelength.

We used the owner of spectra of supernovæ built using a collection of spectra observed with various phases built by nugent2002.

In general, the spectra observed are not usable directly to make spectrophotometry. Indeed, the atmosphere plays the role of prism and disperses in a differential way the various wavelengths. This effect has a continuous dependence in wavelength and can be corrected by the photometric observation of the same object.

In our case, the spectra were standardized so as to reproduce the colors observed of the supernovæ.

The method of construction of this owner is detailed in nugent2002. We will use in the continuation the modified owners of spectrum knop2003. This owner was standardized so as to reproduce the colors observed in UBVRI of supernovæ close exits of the literature.

Figure 9.3: This figure represents the owner of spectra built by nugent2002. Are represented a spectrum per week as from 2 weeks before the maximum of luminosity up to 4 weeks afterwards.

Figure 9.3 shows the owner built nugent2002 with a one week sampling.

The owner that we use has been composed of 90 spectra standardized for 20 days front up to 70 days after the maximum of luminosity out of B.

It finally was standardized to reproduce the intrinsic luminosity definite by equation 2.18 and was measured by jha1999: $63.4 \rm \, km\, s^{-1 } \, { \rm Mpc^{-1}}$.

The last stage of the construction of the lightcurves is the taking into account of the distance and the redshift which are bound by cosmology.