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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1630.fig1.eps}\end{figure}$ Figure 1: Hubble constant as a function of $\rm ^{56}Ni$ mass for 12 SNe Ia in the Hubble flow for $\alpha$ = 1. Error bars represent all uncertainties discussed in Sect. 4.1. The dotted lines indicate the two $\rm ^{56}Ni$ masses from our adopted models. The solid vertical line indicates an upper limit on the production of $\rm ^{56}Ni$ expected from the thermonuclear explosion of a C-O white dwarf, and the solid horizontal line corresponds to the lower limit we derive for H₀.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1630.fig2.eps}\end{figure}$ Figure 2: To highlight the absolute lower limit we derive on H₀ we plot results obtained with SN 1999aa (the least luminous of our 10 normal SNe Ia) with 1- $\sigma$ (dark shading) and 3- $\sigma$ (light shading) confidence levels. Vertical solid lines indicate both the adopted $\rm ^{56}Ni$ masses and the 1 $M_{\odot }$ upper limit expected from an exploding C-O white dwarf. The dashed line illustrates the effect if $\alpha$ is increased by 20% (i.e. $\alpha$ = 1.2).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1630.fig3.eps}\end{figure}$ Figure 3: Hubble diagram of 12 SNe Ia in the Hubble flow. The negative logarithm of the UVOIR flux at maximum light is plotted against the logarithm of the recession velocity in the CMB frame. Error bars account for a peculiar velocity of 400 km s^-1 and uncertainties associated with host galaxy reddening.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1630.fig3.eps}\end{figure}$	Figure 3: Hubble diagram of 12 SNe Ia in the Hubble flow. The negative logarithm of the UVOIR flux at maximum light is plotted against the logarithm of the recession velocity in the CMB frame. Error bars account for a peculiar velocity of 400 km s^-1 and uncertainties associated with host galaxy reddening.
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