All Figures

$\begin{figure} \par\includegraphics[height=6.4cm,width=8.2cm,clip]{9796fig1.eps} \end{figure}$ Figure 1: Distribution of the number of stellar populations recovered by VESPA from the host sample (gray) and the control sample (white). The two distributions are very similar (see text).
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{9796fig2.eps} \end{figure}$ Figure 2: Type Ia supernova rate per stellar mass, unnormalized, vs. fraction of stellar mass formed in the four time intervals indicated in each panel. The dashed line is a fit to a dual component model ${\it SNR} = \alpha \times M_*+ \beta \times M_{\rm time\ range}$ , for each time range. In the absence of a stellar population of a given age contributing to the supernova rate, the curve would be consistent with flat (i.e., $\beta$ consistent with zero). We find that $\beta /\alpha$ is non zero at the five-sigma level for the time intervals [0-180] Myr. Shaded areas are $\pm$ $2\sigma$ fit values.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{9796fig3.eps} \end{figure}$ Figure 3: Estimation of the possible bias that can be introduced by star formation today taking place preferentially in smaller mass galaxies. Using our SDSS control sample we have generated supernova using $\beta /\alpha = 0$ and $\beta /\alpha = 700$ . The recovered lines show that for the case with $\beta /\alpha = 0$ (dotted line) we indeed find no signature of supernova, while for the case $\beta /\alpha = 700$ we do recover supernova activity at the 2/3 level (dotted line) of the input value ( $\beta /\alpha \simeq 465$ ), thus our conclusions are conservative. See more details in text.
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In the text

$\begin{figure} \par\includegraphics[height=6.4cm,width=8.2cm,clip]{9796fig1.eps} \end{figure}$	Figure 1: Distribution of the number of stellar populations recovered by VESPA from the host sample (gray) and the control sample (white). The two distributions are very similar (see text).
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