All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f1.ps} \end{figure}$ Figure 1: Redshift $z_{\rm f}$ from ${\cal SN}$ -fit as a function of the redshift $z_{\rm h}$ of the host galaxy ( top panel), and residuals ( bottom panel). Error bars shown are for the host redshift only.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3552f16.eps} \end{figure}$ Figure 16: Heavily smoothed spectra of the eight pre-maximum SN Ia of the intermediate redshift sample ordered in a sequence of increasing phase (logarithmic scale). Spectra are shifted by an arbitrary amount for visual convenience, and are shown into the restframe. Atmospheric absorptions and galaxy line subtractions have been removed before smoothing. Grey vertical bands show the Ca II, S II and Si II features found in normal SN Ia. Solid vertical lines show the positions of Ca II at 3945 Å, S II at 5640 Å $\$ and Si II at 6355 Å $\$ , blueshifted by 15 000 km s^-1 (Ca II) and 10 000 km s^-1 (S II, Si II). These values are typical of "normal'' SN Ia at maximum and are shown as a guide to the eye.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3552f17.eps} \end{figure}$ Figure 17: Same as Fig. 16 for the six past-maximum SN Ia (including the two NOT spectra) of the intermediate redshift sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f18.ps} \end{figure}$ Figure 18: Ca II velocity as a function of B-band phase. Data are taken from Fig. 11 of Benetti et al.(2004). Calcium velocities for the SN Ia presented in this paper (plotted as filled circles) are given in Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f19.ps} \end{figure}$ Figure 19: Comparison of best fits obtained for "normal'' and peculiar SN Ia templates for two low S/N ratio supernovae for which identification might be questionable. Top: SN 1999gx, and bottom: SN 1999cj. For clarity, peculiar solutions have been shifted by an arbitrary amount in y-scale. In both cases, visual inspection slightly favors the normal solution over the peculiar one.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f20.ps} \end{figure}$ Figure 20: Photometric phase relative to spectroscopic phase for the five photometrically followed-up SN Ia of our sample ( top panel), and residuals ( bottom panel). Errors shown are for the photometric phase only and assume a conservative $\pm$ 1 day error. The photometric phase is from fit of the restframe B-band light-curve and the spectroscopic phase from $\chi ^2$ minimization fitting of observed spectra with SN Ia spectral templates.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f2.ps} \end{figure}$ Figure 2: Top: SN 1999cj+host in the observer frame. Bottom: Galaxy-subtracted SN 1999cj, rebinned for visual convenience, with the best-fit template (SN 1992A +9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. Note the restframe UV part accessible due to the use of ISIS blue arm for this supernova.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f3.ps} \end{figure}$ Figure 3: Top: WHT spectrum of SN 1999cj+host in the observer frame. Bottom: rebinned galaxy-subtracted spectrum of SN 1999ck with the best-fit template (SN 1994D -9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. As for SN 1999cj, the restframe UV part is visible due to the use of ISIS blue arm.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f4.ps} \end{figure}$ Figure 4: Top: WHT spectrum of SN 1999dr host galaxy alone. Bottom: rebinned galaxy-subtracted spectrum SN 1999dr with the best-fit template (SN 1994D + 24 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f5.ps} \end{figure}$ Figure 5: Top: WHT spectrum of SN 1999dt+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dt with the best-fit template (SN 1994D -9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. Note the poor [O II], H $_\beta$ and H $_\gamma$ line subtraction and the presence of strong atmospheric absorptions.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f6.ps} \end{figure}$ Figure 6: Top: WHT spectrum of SN 1999du+host. Bottom: rebinned galaxy subtracted spectrum of SN 1999du with the best-fit template (SN 1999ee -9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f7.ps} \end{figure}$ Figure 7: Top: NOT spectrum of SN 1999du host alone. Due to the presence of the second order in the NOT spectra, the signal beyond $\sim$ 6000 Å $\$ is distorted and can not be used in the identification fitting procedure. It however shows the presence of galaxy lines (H $_\beta$ in this case) useful for redshift determination. Bottom: rebinned galaxy subtracted spectrum of SN 1999du with the best-fit template (SN 1992A +6 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. The spectral range of the bottom panel does not match the one of the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f8.ps} \end{figure}$ Figure 8: WHT spectrum of SN 1999dv+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dv with the best-fit template (SN 2003du -7 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions and galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f9.ps} \end{figure}$ Figure 9: Top: NOT spectrum of SN 1999dv+host. Due to the presence of the second order in the NOT spectra, the signal beyond $\sim$ 6000 Å $\$ is distorted and can not be used in the identification fitting procedure. It however shows the presence of galaxy lines useful for redshift determination. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dv with the best-fit template (SN 1992A +9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. The spectral range of the bottom panel does not match the one of the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f10.ps} \end{figure}$ Figure 10: Top: WHT spectrum of SN 1999dw+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dw with the best-fit template (SN 1999ee -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f11.ps} \end{figure}$ Figure 11: Top: WHT spectrum of SN 1999dx+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dx with the best-fit template (SN 1992A +5 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals. Note the presence of strong atmospheric absorptions and a narrow absorption-like feature at 5900 Å $\$ in the SN 1992A +5 days template.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f12.ps} \end{figure}$ Figure 12: Top: WHT spectrum of SN 1999dy+host. Bottom: Rebinned galaxy-subtracted spectrum of SN 1999dy with the best-fit template (SN 1996X 0 day) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f13.ps} \end{figure}$ Figure 13: Top: WHT spectrum of SN 1999dz+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dz with the best-fit template (SN 1999ee -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f14.ps} \end{figure}$ Figure 14: Top: WHT spectrum of SN 1999ea+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999ea with the best-fit template (SN 1994D -8 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f15.ps} \end{figure}$ Figure 15: Top: WHT spectrum of SN 1999gx+host. Bottom: Rebinned galaxy-subtracted spectrum of SN 1999gx with the best-fit template (SN 1994D -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{3552f21.ps} \end{figure}$ Figure 21: WFS reference images of host galaxies. Each vignette is a $0.25\times 0.25$ square-arcmin cutout of the full CCD, centered on the position where the SN exploded (indicated by a cross). All images are in $g\hbox {$^\prime $ }$ , except for SN 1999cj (B image) and SN 1999ck ( $r\hbox {$^\prime $ }$ image).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3552f22.ps} \end{figure}$ Figure A.1: Phase distribution of type Ia templates in ${\cal SN}$ -fit database. Up: normal SN Ia . Middle: 91bg-like SN Ia . Bottom: 91T-like SN Ia.

In the text

$\begin{figure} \par\includegraphics[width=10.8cm,clip]{3552f23.ps} \end{figure}$ Figure A.2: Phase distribution of type Ib, Ic and II templates in ${\cal SN}$ -fit database.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f1.ps} \end{figure}$	Figure 1: Redshift $z_{\rm f}$ from ${\cal SN}$ -fit as a function of the redshift $z_{\rm h}$ of the host galaxy ( top panel), and residuals ( bottom panel). Error bars shown are for the host redshift only.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3552f17.eps} \end{figure}$	Figure 17: Same as Fig. 16 for the six past-maximum SN Ia (including the two NOT spectra) of the intermediate redshift sample.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f18.ps} \end{figure}$	Figure 18: Ca II velocity as a function of B-band phase. Data are taken from Fig. 11 of Benetti et al.(2004). Calcium velocities for the SN Ia presented in this paper (plotted as filled circles) are given in Table 3.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3552f19.ps} \end{figure}$	Figure 19: Comparison of best fits obtained for "normal'' and peculiar SN Ia templates for two low S/N ratio supernovae for which identification might be questionable. Top: SN 1999gx, and bottom: SN 1999cj. For clarity, peculiar solutions have been shifted by an arbitrary amount in y-scale. In both cases, visual inspection slightly favors the normal solution over the peculiar one.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f4.ps} \end{figure}$	Figure 4: Top: WHT spectrum of SN 1999dr host galaxy alone. Bottom: rebinned galaxy-subtracted spectrum SN 1999dr with the best-fit template (SN 1994D + 24 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f6.ps} \end{figure}$	Figure 6: Top: WHT spectrum of SN 1999du+host. Bottom: rebinned galaxy subtracted spectrum of SN 1999du with the best-fit template (SN 1999ee -9 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f8.ps} \end{figure}$	Figure 8: WHT spectrum of SN 1999dv+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dv with the best-fit template (SN 2003du -7 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions and galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f10.ps} \end{figure}$	Figure 10: Top: WHT spectrum of SN 1999dw+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dw with the best-fit template (SN 1999ee -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f12.ps} \end{figure}$	Figure 12: Top: WHT spectrum of SN 1999dy+host. Bottom: Rebinned galaxy-subtracted spectrum of SN 1999dy with the best-fit template (SN 1996X 0 day) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f13.ps} \end{figure}$	Figure 13: Top: WHT spectrum of SN 1999dz+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999dz with the best-fit template (SN 1999ee -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f14.ps} \end{figure}$	Figure 14: Top: WHT spectrum of SN 1999ea+host. Bottom: rebinned galaxy-subtracted spectrum of SN 1999ea with the best-fit template (SN 1994D -8 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=12.5cm,clip]{3552f15.ps} \end{figure}$	Figure 15: Top: WHT spectrum of SN 1999gx+host. Bottom: Rebinned galaxy-subtracted spectrum of SN 1999gx with the best-fit template (SN 1994D -4 days) overlapped. The spectrum is shown in the observer frame and is not corrected for atmospheric absorptions or galactic line subtraction residuals.
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$\begin{figure} \par\includegraphics[width=10cm,clip]{3552f21.ps} \end{figure}$	Figure 21: WFS reference images of host galaxies. Each vignette is a $0.25\times 0.25$ square-arcmin cutout of the full CCD, centered on the position where the SN exploded (indicated by a cross). All images are in $g\hbox {$^\prime $ }$ , except for SN 1999cj (B image) and SN 1999ck ( $r\hbox {$^\prime $ }$ image).
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