$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig1.ps} \end{figure}$ Figure 1: Visible spectra of 9 objects taken before April 2007 with the old detector of FORS1. Spectra are shifted vertically by 0.57 for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig2.ps} \end{figure}$ Figure 2: Visible spectra of 9 objects taken after April 2007 with the new detector of FORS1. Spectra are shifted vertically by 0.57 for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig6.ps} \end{figure}$ Figure 6: S-Distributions for the complete sample ( top), Centaurs plus detached plus scattered disk objects ( middle), and classical plus resonant objects ( bottom). The chosen bin was 2% (0.1 $\mu$ m)^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9705fig7.ps}\par\includegraphics[width=7.5cm,clip]{9705fig8.ps} \end{figure}$ Figure 7: a) Spectra of 2003 AZ₈₄ after removal of the continuum (see text). b) Spectra of 42 355 Typhon and 10 199 Chariklo after removal of the continuum.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig1.ps} \end{figure}$	Figure 1: Visible spectra of 9 objects taken before April 2007 with the old detector of FORS1. Spectra are shifted vertically by 0.57 for clarity.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig2.ps} \end{figure}$	Figure 2: Visible spectra of 9 objects taken after April 2007 with the new detector of FORS1. Spectra are shifted vertically by 0.57 for clarity.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9705fig3.ps} \end{figure}$	Figure 3: Visible spectra of 83 982 Crantor. Spectra are shifted vertically by 0.55.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9705fig4.ps} \end{figure}$	Figure 4: Visible spectra of 47 932 (2000 GN₁₇₁). Spectra are shifted vertically by 0.55.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9705fig5.ps} \end{figure}$	Figure 5: Visible spectra of the dwarf planet 136 199 Eris. Spectra are shifted vertically by 1.0.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{9705fig6.ps} \end{figure}$	Figure 6: S-Distributions for the complete sample ( top), Centaurs plus detached plus scattered disk objects ( middle), and classical plus resonant objects ( bottom). The chosen bin was 2% (0.1 $\mu$ m)^-1.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9705fig7.ps}\par\includegraphics[width=7.5cm,clip]{9705fig8.ps} \end{figure}$	Figure 7: a) Spectra of 2003 AZ₈₄ after removal of the continuum (see text). b) Spectra of 42 355 Typhon and 10 199 Chariklo after removal of the continuum.
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