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The batch

Close supernovæ that we used come mainly from the research carried out within the framework of Calàn-Tololo Supernovae Survey (hamuy1996c), of CFA between 1993 and 1996 (riess1999), and between 1997 and 2000 (jha2002). We added to this batch about fifteen supernovæ resulting from various bibliographical sources.

The characteristics of these supernovæ are detailed in C.1 table .

The redshifts (observed and corrected for the movement of our galaxy compared to the CMB) and excesses of Galactique color ( $ E(b-v)$ ) were given thanks to the astronomical search engine NED . We, for checking, calculated the values of excesses of color by using the charts of Galactiques dust resulting from schlegel1998, we checked that the values are quite identical.

Figures 10.3 present the distributions of the redshifts, color ( $ -0.25 < (B-v)_{max } < 1.6$ ) and a panel of factor of stretching ranging between 0.6 and 1.2.

Appear: Distribution of the redshifts for the close supernovæ used in this analysis.
\begin{figure}\it\begin{center} \epsfig{file=Images/RedshiftDistribNear.eps, width=12cm}\end{center}\end{figure}

Figure 10.2: Distribution of the colors for the close supernovæ used in this analysis.
\begin{figure}\it\begin{center} \epsfig{file=Images/BVDistribNear.eps, width=12cm}\end{center}\end{figure}

Figure 10.3: Distribution of the factors of stretching for the close supernovæ used in this analysis.
\begin{figure}\it\begin{center} \epsfig{file=Images/StretchDistribNear.eps, width=12cm}\end{center}\end{figure}

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Julien Raux 2004-05-04