All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig1.eps} \end{figure}$ Figure 1: Field of SN 2003du. The field of view is $10^\prime \times 10^\prime$ . The stars used as local standards are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig2.eps} \end{figure}$ Figure 2: The $\it UBVRI$ light curves of SN 2003du. The abscissae correspond to days since B maximum. The errorbars in magnitude are less than or comparable to the point size.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig3.eps} \end{figure}$ Figure 3: U, B, V, R and I light curves of SNe 2003du, 1991T, 1990N, 1998bu and 1994D. The ordinate in each panel is the magnitude below the respective maximum, and the abscissae represent the days since respective B maximum.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig4.eps} \end{figure}$ Figure 4: The U-B, B-V, V-R and R-I colour curves of SN 2003du. Also shown for a comparison are the colour curves of SNe 1991T, 1990N, 1998bu and 1994D. The abscissae correspond to days since respective B maximum.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig5.eps} \end{figure}$ Figure 5: The bolometric light curve of SN 2003du.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig6.eps} \end{figure}$ Figure 6: The spectral evolution of SN 2003du from phase -11 d to +9 d. The spectra are not corrected for reddening. For clarity, the spectra have been displaced vertically. Dotted lines at the left indicate the zero flux level for each spectrum. For +9 d, zero flux is the x-axis. Wavelength scale is in the observer rest frame. Main line identifications are marked according to Mazzali et al. (1993).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig7.eps} \end{figure}$ Figure 7: The spectral evolution of SN 2003du from phase +13 d to +37 d. The spectra are not corrected for reddening. For clarity, the spectrum of +13d has been displaced vertically and the dotted line at the left indicates the zero flux level. The zero flux for +37 d is the x-axis. Wavelength scale is in the observer rest frame. Main line identifications are marked according to Mazzali et al. (1993).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig8.eps} \end{figure}$ Figure 8: The spectral evolution of SN 2003du from phase +87 d to +139 d. The spectra are not corrected for reddening. For clarity, the spectra have been displaced vertically. Dotted lines at the left indicate the zero flux level for each spectrum. For +139 d, zero flux is the x-axis. Wavelength scale is in the observer rest frame. Main line identifications are marked according to Bowers et al. (1997).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig9.eps} \end{figure}$ Figure 9: Comparison between the observed spectra of SN 2003du and SN 1990N on day -7. The spectrum of SN 1990N was obtained from http://hej3.as.utexas.edu/~www/SN/spec/sn1a/90N/. The flux units are arbitrary, and the wavelength scale is corrected for the recession velocity of the respective parent galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig10.eps} \end{figure}$ Figure 10: Expansion velocities derived from the absorption minima of Si II 6355 Å and the Ca II H and K for SN 2003du, SN 1994D, SN 1990N and SN 1996X (see text for references). The Ca II IR-triplet absorption velocities are also plotted for SN 2003du (stars). The expansion velocities have been corrected for the recession velocity of the host galaxy. The vertical lines connect the low and the high velocity components of the Ca II absorption in SN 2003du when both components were detected.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig1.eps} \end{figure}$	Figure 1: Field of SN 2003du. The field of view is $10^\prime \times 10^\prime$ . The stars used as local standards are listed in Table 1.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig2.eps} \end{figure}$	Figure 2: The $\it UBVRI$ light curves of SN 2003du. The abscissae correspond to days since B maximum. The errorbars in magnitude are less than or comparable to the point size.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig3.eps} \end{figure}$	Figure 3: U, B, V, R and I light curves of SNe 2003du, 1991T, 1990N, 1998bu and 1994D. The ordinate in each panel is the magnitude below the respective maximum, and the abscissae represent the days since respective B maximum.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{1687fig4.eps} \end{figure}$	Figure 4: The U-B, B-V, V-R and R-I colour curves of SN 2003du. Also shown for a comparison are the colour curves of SNe 1991T, 1990N, 1998bu and 1994D. The abscissae correspond to days since respective B maximum.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig5.eps} \end{figure}$	Figure 5: The bolometric light curve of SN 2003du.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1687fig9.eps} \end{figure}$	Figure 9: Comparison between the observed spectra of SN 2003du and SN 1990N on day -7. The spectrum of SN 1990N was obtained from http://hej3.as.utexas.edu/~www/SN/spec/sn1a/90N/. The flux units are arbitrary, and the wavelength scale is corrected for the recession velocity of the respective parent galaxy.
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