All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4506f1N.eps}\end{figure}$ Figure 1: One IRTF image of Saturn taken in J band on October 6th, 2000, showing the position of the slit ( $0.5\times 15$ arcsec²) on the west ansa.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4506f2N.eps}\end{figure}$ Figure 2: A part of the mode 1 coverage of the 1 $\mu$ m region obtained with the slit on the rings as shown in Fig. 1. The direction of wavelength dispersion is indicated by $\lambda$ . The adjacent partial band is a piece of the next wavelength range, which lies adjacent on the CCD.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{h4506.f3.eps} \end{figure}$ Figure 3: Spectra of B and A rings at two different phase angles. The water ice absorption bands in the 0.9-2.5 $\mu$ m range are indicated with vertical lines.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{h4506.f4.eps} \end{figure}$ Figure 4: Upper: Smoothed ratio of spectra of B/A. The ratio is normalized to 1 at 1 $\mu$ m. Lower: Smoothed ratio of spectra of C/B compared to a terrestrial and natural organic. The curves are normalized to 1 at 3.9 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{h4506.f5.eps} \end{figure}$ Figure 5: Spectrum of C ring obtained at 4.7 ${}^\circ$ phase angle. The water ice absorption bands in the 0.9-2.5 $\mu$ m range are indicated with vertical lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4506.f6.eps} \end{figure}$ Figure 6: Comparison of the 2.95-3.2 $\mu$ m spectra of the C ring (solid) and several icy satellites with amorphous water ice (upper) and crystalline water ice (lower). A continuum determined by fitting a least squares polynomial curve 2.85-3.3 points at the ends of the spectral range is subtracted. The spectra shown include calculated spectrum of amorphous frost, laboratory reflectance of crystalline water ice (Roush et al. 1990), spectra of Europa (McCord et al. 1999), and Callisto, Rhea (Dalle Ore 2002, personal communication).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f7.eps} \end{figure}$ Figure 7: Spectra of the B ring taken at 4.7 ${}^\circ$ phase angle compared with its model (red curve). No significant difference between East and West ansa is observed. See Table 2 for a description of the model.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f8.eps} \end{figure}$ Figure 8: Spectrum of the A ring taken at 4.7 ${}^\circ$ phase angle compared with its model (red curve). No significant difference between East and West ansa is observed. See Table 3 for a description of the model.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f9.eps} \end{figure}$ Figure 9: Spectrum of the C ring compared with three models (red, green and blue curves). Red: best model; blue: same as red except for one water ice grain made of amorphous water ice; green: Same kind of mixture than that used for the spectra of the B and A rings.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{h4506.f10.eps} \end{figure}$ Figure 10: Data/model ratio for B (upper) and A rings (lower).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{h4506.f11.eps} \end{figure}$ Figure 11: Data/model ratio for C ring.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4506f1N.eps}\end{figure}$	Figure 1: One IRTF image of Saturn taken in J band on October 6th, 2000, showing the position of the slit ( $0.5\times 15$ arcsec²) on the west ansa.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4506f2N.eps}\end{figure}$	Figure 2: A part of the mode 1 coverage of the 1 $\mu$ m region obtained with the slit on the rings as shown in Fig. 1. The direction of wavelength dispersion is indicated by $\lambda$ . The adjacent partial band is a piece of the next wavelength range, which lies adjacent on the CCD.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{h4506.f3.eps} \end{figure}$	Figure 3: Spectra of B and A rings at two different phase angles. The water ice absorption bands in the 0.9-2.5 $\mu$ m range are indicated with vertical lines.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{h4506.f4.eps} \end{figure}$	Figure 4: Upper: Smoothed ratio of spectra of B/A. The ratio is normalized to 1 at 1 $\mu$ m. Lower: Smoothed ratio of spectra of C/B compared to a terrestrial and natural organic. The curves are normalized to 1 at 3.9 $\mu$ m.
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{h4506.f5.eps} \end{figure}$	Figure 5: Spectrum of C ring obtained at 4.7 ${}^\circ$ phase angle. The water ice absorption bands in the 0.9-2.5 $\mu$ m range are indicated with vertical lines.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f7.eps} \end{figure}$	Figure 7: Spectra of the B ring taken at 4.7 ${}^\circ$ phase angle compared with its model (red curve). No significant difference between East and West ansa is observed. See Table 2 for a description of the model.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f8.eps} \end{figure}$	Figure 8: Spectrum of the A ring taken at 4.7 ${}^\circ$ phase angle compared with its model (red curve). No significant difference between East and West ansa is observed. See Table 3 for a description of the model.
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$\begin{figure} \par\includegraphics[angle=90,width=12cm,clip]{h4506.f9.eps} \end{figure}$	Figure 9: Spectrum of the C ring compared with three models (red, green and blue curves). Red: best model; blue: same as red except for one water ice grain made of amorphous water ice; green: Same kind of mixture than that used for the spectra of the B and A rings.
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$\begin{figure} \par\includegraphics[width=11cm,clip]{h4506.f10.eps} \end{figure}$	Figure 10: Data/model ratio for B (upper) and A rings (lower).
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$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{h4506.f11.eps} \end{figure}$	Figure 11: Data/model ratio for C ring.
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