All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{1256fig1.eps} \end{figure}$ Figure 1: Distribution of $\Delta z = (z_{\rm ph} - z_{\rm sp})/(1+z_{\rm sp})$ , the difference between our estimate of the photometric redshift and a) spectroscopic redshifts, for the 324 galaxies of our sample with known spectroscopic redshift (thin line) and b) COMBO17 photometric redshifts of Wolf et al. (2003) for the 1375 galaxies which are in common with our sample (thick line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1256fig2.eps} \end{figure}$ Figure 2: Redshift distribution of our galaxy sample (line, left-side scale) and SNe host galaxies (dots, right-side scale). For the latter, candidates coincident with the host galaxy nucleus have been counted with a 0.4 weight.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1256fig3.eps} \end{figure}$ Figure 3: Example of SN detection efficiency curve, plotted as a function of apparent magnitude for one of the epochs of field AXAF(seeing $0\hbox{$.\!\!^{\prime\prime}$ }9$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig4.eps} \end{figure}$ Figure 4: Galaxy luminosity density ad different redshifts. Data are from Norberg et al. (2002); Wolf et al. (2003); Madau et al. (1998); Blanton et al. (2003). The line represents the best fit using a $(1+z)^{\alpha }$ power law (see the text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig5.eps} \end{figure}$ Figure 5: Measurements of the SN Ia rate at different redshifts. References are as follows: filled triangle - Cappellaro et al. (1999), filled upside-down triangle - Blanc et al. (2004), filled square - Madgwick et al. (2003), empty square - Hardin et al. (2000), filled circle - Tonry et al. (2003), filled diamond - Pain et al. (2002), empty diamond - Gal-Yam et al. (2002). The line is a fit with the power law in (1+z) (see the text for details). Because of the large errorbars the Gal-Yam et al. estimates have not be used for the fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig6.eps} \end{figure}$ Figure 6: Confidence level for the maximum-likelihood test.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig7.eps} \end{figure}$ Figure 7: Observed (points with statistical errorbars) and expected (solid line) redshift distribution of SN counts. The short-dashed and long-dashed lines are the expected type Ia and CC SN counts respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig8.eps} \end{figure}$ Figure 8: CC SN rate with redshift. The dot is the estimate of the local CC SN rate from Cappellaro et al. (1999) whereas the square is the new measurement derived in this paper. The solid line shows the deduced evolution with redshift. The dashed line shows the deduced type Ia rate evolution (see the text for details). The thick solid line is the CC SN rate evolution predicted by model M2 of Sadat et al. (1998).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1256fig9.eps} \end{figure}$ Figure 9: We compare our estimate of the SFR at redshift z=0.26 (big filled dot) with the recent estimate of Fujita et al. (2003) based on the H $\alpha$ luminosity density at z=0.24 (filled square). Also shown are estimates of the SFR at other redshifts based either on measurements of the H $\alpha$ (filled symbols) or of the UV luminosity density (adapted from Fujita et al. (2003) and reference therein). Also plotted is the value derived from the local CC rate (also big filled dot).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{1256fig1.eps} \end{figure}$	Figure 1: Distribution of $\Delta z = (z_{\rm ph} - z_{\rm sp})/(1+z_{\rm sp})$ , the difference between our estimate of the photometric redshift and a) spectroscopic redshifts, for the 324 galaxies of our sample with known spectroscopic redshift (thin line) and b) COMBO17 photometric redshifts of Wolf et al. (2003) for the 1375 galaxies which are in common with our sample (thick line).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1256fig2.eps} \end{figure}$	Figure 2: Redshift distribution of our galaxy sample (line, left-side scale) and SNe host galaxies (dots, right-side scale). For the latter, candidates coincident with the host galaxy nucleus have been counted with a 0.4 weight.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1256fig3.eps} \end{figure}$	Figure 3: Example of SN detection efficiency curve, plotted as a function of apparent magnitude for one of the epochs of field AXAF(seeing $0\hbox{$.\!\!^{\prime\prime}$ }9$ ).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig4.eps} \end{figure}$	Figure 4: Galaxy luminosity density ad different redshifts. Data are from Norberg et al. (2002); Wolf et al. (2003); Madau et al. (1998); Blanton et al. (2003). The line represents the best fit using a $(1+z)^{\alpha }$ power law (see the text for details).
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig6.eps} \end{figure}$	Figure 6: Confidence level for the maximum-likelihood test.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{1256fig7.eps} \end{figure}$	Figure 7: Observed (points with statistical errorbars) and expected (solid line) redshift distribution of SN counts. The short-dashed and long-dashed lines are the expected type Ia and CC SN counts respectively.
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