All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig1.eps}\par\includegraphics[width=8cm,clip]{2463fig2.eps}\end{figure}$ Figure 1: I-band light curve fits. On the ordinate is the flux normalised to the first peak, on the abscissa the restframe time since B-band maximum. The dashed line and the dash-dotted line represent the two templates used to fit the first and second peak respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig3.eps}\par\includegraphics[width=8cm,clip]{2463fig4.eps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig5.eps}\par\includegraphics[width=8cm,clip]{2463fig6.eps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig7.eps}\par\includegraphics[width=8cm,clip]{2463fig8.eps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig9.eps}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{2463fig10.eps}\includegraphics[width=4cm,clip]{2463fig11.eps}\end{figure}$ Figure 2: Distribution of the time of I-band maximum referred to the time of B-band maximum ( left panel) and the distribution of the time of second maximum referred to the time of B-band maximum ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig12.eps}\end{figure}$ Figure 3: I-band absolute magnitude versus stretch in the B-band. The best fit gives $\alpha _I = 1.18 \pm 0.19$ and $M_{\rm max}^I(s_B=1)=-18.84 \pm 0.03$ mag. The two deviating supernovae, SN 1998es (filled diamond) and SN 1999dq (filled circle), were excluded from the fit.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig13.eps}\end{figure}$ Figure 4: Time since $B_{\rm max}$ of the second peak versus the stretch in the B-band. The labelled supernovae, classified as spectroscopically peculiar, are excluded from the fit because they are outliers.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig14.eps}\end{figure}$ Figure 5: Absolute magnitude of the secondary peak versus the stretch in the B-band. The two deviating supernovae in Fig. 3 are SN 1998es (filled diamond) and SN 1999dq (filled circle).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig15.eps}\end{figure}$ Figure 6: I-band light curve stretch, s_I, versus B-band stretch, s_B. The labelled supernovae are more than two standard deviation from the correlation shown by the ensemble. SN 1998ab, SN 1997br and SN 1998es are classified as spectroscopically peculiar.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2463fig16.eps}\end{figure}$ Figure 7: Effective I-band maximum vs. redshift for the nearby supernovae of the Calan/Tololo, CfA and CfA2 sample. The data have been corrected for the stretch-luminosity relation and for Milky Way and host galaxy extinction. The rms along the concordance model line is $\sigma =0.17$ $\pm$ 0.04 mag. Subtracting the contribution of the average uncertainty, results in 0.13 mag estimated intrinsic dispersion (see text for details). SN 1998es and SN 1999dq were excluded from the fit (see text) and are plotted with open diamonds. The inset plots the histogram of the residuals.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{2463fig17.eps}\end{figure}$ Figure 8: Comparison between the Persson Jfilter (dashed-dotted line), the J_s filter at ISAAC used for the observations of SN 2000fr (dashed line) and the I-band red-shifted to z= 0.543 (heavy solid line). The atmospheric transmission is also plotted (dotted line). The spectral template at day 0 is on an arbitrary flux scale for readability purpose (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig18.eps}\end{figure}$ Figure 9: I-band fit for SN 2000fr. Out of 42 I-band templates, the best fit was obtained with the template of SN 1992bc. The fit was performed with only one free parameter, the peak magnitude, $I_{\rm max}=23.48$ $\pm$ 0.08 mag. Supplemental data from the B-band (not shown) is used to fix the date of B-maximum.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig19.eps}\end{figure}$ Figure 10: I-band fit for SN 1999ff. Out of 42 I-band templates, the best fit was obtained with the template of SN 1996bl. The fit was performed with only one free parameter, the peak magnitude, $I_{\rm max}=23.55$ $\pm$ 0.10 mag. Supplemental data from the B-band (not shown) is used to fix the date of B-maximum.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2463fig20.eps}\end{figure}$ Figure 11: Effective I-band maximum versus redshift for the nearby supernovae of the Calan/Tololo, CfA and CfA2 sample, together with two supernovae at redshift $\sim$ 0.5 for case c ( top panel), residuals to the ( $\Omega_{\rm M},\;\Omega_\Lambda$ ) = (0.25, 0.75) model for case c ( middle panel) and case a ( bottom panel). SN 1998es and SN 1999dq were excluded from the fit (see text) and are plotted with open diamonds. Only the low-redshift SNe have been extinction corrected. The host galaxy extinction correction would make the two high-redshift data points closer to each other but with larger error bars.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig21.eps}\par\includegraphics[width=8cm,clip]{2463fig22.eps}\end{figure}$ Figure 12: The evolution in the colour of SN 1999ff (squares) and SN 2000fr (triangles), B-V ( top panel) and B-I ( bottom panel), compared to the colour evolution of the average SNe Ia in a $\Lambda$ dominated universe (solid line) and a $\Omega _{\rm M} =1$ , $\Omega _\Lambda =0$ universe with presence of grey dust with R_V = 4.5 (dashed line) and R_V = 9.5 (dotted line) for z=0.5.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig23.eps}\includegraphi... ...,clip]{2463fig25.eps}\includegraphics[width=8cm,clip]{2463fig26.eps}\end{figure}$ Figure 13: Left-hand panels: distribution of combined colour measurements of nearby SNe Ia in the E(B-I) vs. E(B-V) plane, not corrected ( top panel) and corrected ( bottom panel) for the host galaxy extinction. The solid contours incorporate 68.3%, 95.5% and 99.7% of the sample. Right-hand panels: SN 1999ff and SN 2000fr compared to the distribution defined by nearby SNe in the case of no IG dust (solid ellipses), and in the case of IG dust with R_V=9.5 (dashed ellipse). For clarity only the 68.3% level has been plotted for the dust distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig1.eps}\par\includegraphics[width=8cm,clip]{2463fig2.eps}\end{figure}$	Figure 1: I-band light curve fits. On the ordinate is the flux normalised to the first peak, on the abscissa the restframe time since B-band maximum. The dashed line and the dash-dotted line represent the two templates used to fit the first and second peak respectively.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig3.eps}\par\includegraphics[width=8cm,clip]{2463fig4.eps}\end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=4cm,clip]{2463fig10.eps}\includegraphics[width=4cm,clip]{2463fig11.eps}\end{figure}$	Figure 2: Distribution of the time of I-band maximum referred to the time of B-band maximum ( left panel) and the distribution of the time of second maximum referred to the time of B-band maximum ( right panel).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig12.eps}\end{figure}$	Figure 3: I-band absolute magnitude versus stretch in the B-band. The best fit gives $\alpha _I = 1.18 \pm 0.19$ and $M_{\rm max}^I(s_B=1)=-18.84 \pm 0.03$ mag. The two deviating supernovae, SN 1998es (filled diamond) and SN 1999dq (filled circle), were excluded from the fit.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig13.eps}\end{figure}$	Figure 4: Time since $B_{\rm max}$ of the second peak versus the stretch in the B-band. The labelled supernovae, classified as spectroscopically peculiar, are excluded from the fit because they are outliers.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig14.eps}\end{figure}$	Figure 5: Absolute magnitude of the secondary peak versus the stretch in the B-band. The two deviating supernovae in Fig. 3 are SN 1998es (filled diamond) and SN 1999dq (filled circle).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2463fig15.eps}\end{figure}$	Figure 6: I-band light curve stretch, s_I, versus B-band stretch, s_B. The labelled supernovae are more than two standard deviation from the correlation shown by the ensemble. SN 1998ab, SN 1997br and SN 1998es are classified as spectroscopically peculiar.
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{2463fig17.eps}\end{figure}$	Figure 8: Comparison between the Persson Jfilter (dashed-dotted line), the J_s filter at ISAAC used for the observations of SN 2000fr (dashed line) and the I-band red-shifted to z= 0.543 (heavy solid line). The atmospheric transmission is also plotted (dotted line). The spectral template at day 0 is on an arbitrary flux scale for readability purpose (solid line).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig18.eps}\end{figure}$	Figure 9: I-band fit for SN 2000fr. Out of 42 I-band templates, the best fit was obtained with the template of SN 1992bc. The fit was performed with only one free parameter, the peak magnitude, $I_{\rm max}=23.48$ $\pm$ 0.08 mag. Supplemental data from the B-band (not shown) is used to fix the date of B-maximum.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig19.eps}\end{figure}$	Figure 10: I-band fit for SN 1999ff. Out of 42 I-band templates, the best fit was obtained with the template of SN 1996bl. The fit was performed with only one free parameter, the peak magnitude, $I_{\rm max}=23.55$ $\pm$ 0.10 mag. Supplemental data from the B-band (not shown) is used to fix the date of B-maximum.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2463fig21.eps}\par\includegraphics[width=8cm,clip]{2463fig22.eps}\end{figure}$	Figure 12: The evolution in the colour of SN 1999ff (squares) and SN 2000fr (triangles), B-V ( top panel) and B-I ( bottom panel), compared to the colour evolution of the average SNe Ia in a $\Lambda$ dominated universe (solid line) and a $\Omega _{\rm M} =1$ , $\Omega _\Lambda =0$ universe with presence of grey dust with R_V = 4.5 (dashed line) and R_V = 9.5 (dotted line) for z=0.5.
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