All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig1.ps}\end{figure}$ Figure 1: The colour-magnitude diagram of the 42' $\times$ 28' CFH12K field centered on NGC 147. Only stars with $\sigma _{(R-I)}<0.1$ are plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig2.ps}\par\end{figure}$ Figure 2: The colour-colour diagram of same field shown in Fig. 1. Only stars with $\epsilon <0.125$ are plotted (see text). The two boxes define the samples of C and M stars.
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In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{0024fig3.ps}\end{figure}$ Figure 3: Map of the CFH12K fields with all stars with good photometry. C stars are represented by large dots.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig4.ps}\end{figure}$ Figure 4: Luminosity function of C stars in NGC 147.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0024fig5.ps}\end{figure}$ Figure 5: Colour and magnitude comparisons between the C stars discovered in this survey and the ones identified by Nowotny et al. (2003). The upper panel compares the (R-I) colour distributions revealing the different blue limits. The lower panel contrasts the luminosity functions. The dotted histogram is the Nowotny sample. The shaded area corresponds to their C stars with (V-I)₀ < 1.75, too blue to be included in our list.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig6.ps}\end{figure}$ Figure 6: Outer density profile of NGC 147 reaches a plateau at a major axis distance of $\sim$ 25'. The dashed line corresponds to the mean density of the last eleven points. We adopt this value for the foreground density toward NGC 147.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig7.ps}\end{figure}$ Figure 7: The density profile of NGC 147 can be fitted to a power law with a scale length of 4.07'.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0024fig8.ps}\end{figure}$ Figure 8: The stellar density in the periphery of NGC 147 fits well the King relation to evaluate the tidal radius.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{0024fig9.ps}\end{figure}$ Figure 9: The surface density profile of C stars fits the same power law than the old stellar population of NGC 147.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig10.ps}\end{figure}$ Figure 10: Comparison of the foreground I-luminosity function for TNG and CFHT data.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig11.ps}\end{figure}$ Figure 11: Panel a): C/M foreground corrected versus galactocentric distance; Panel b): corresponding [Fe/H] radial gradient (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig1.ps}\end{figure}$	Figure 1: The colour-magnitude diagram of the 42' $\times$ 28' CFH12K field centered on NGC 147. Only stars with $\sigma _{(R-I)}<0.1$ are plotted.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig2.ps}\par\end{figure}$	Figure 2: The colour-colour diagram of same field shown in Fig. 1. Only stars with $\epsilon <0.125$ are plotted (see text). The two boxes define the samples of C and M stars.
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$\begin{figure} \par\includegraphics[width=13.8cm,clip]{0024fig3.ps}\end{figure}$	Figure 3: Map of the CFH12K fields with all stars with good photometry. C stars are represented by large dots.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig4.ps}\end{figure}$	Figure 4: Luminosity function of C stars in NGC 147.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig6.ps}\end{figure}$	Figure 6: Outer density profile of NGC 147 reaches a plateau at a major axis distance of $\sim$ 25'. The dashed line corresponds to the mean density of the last eleven points. We adopt this value for the foreground density toward NGC 147.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig7.ps}\end{figure}$	Figure 7: The density profile of NGC 147 can be fitted to a power law with a scale length of 4.07'.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0024fig8.ps}\end{figure}$	Figure 8: The stellar density in the periphery of NGC 147 fits well the King relation to evaluate the tidal radius.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{0024fig9.ps}\end{figure}$	Figure 9: The surface density profile of C stars fits the same power law than the old stellar population of NGC 147.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0024fig10.ps}\end{figure}$	Figure 10: Comparison of the foreground I-luminosity function for TNG and CFHT data.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0024fig11.ps}\end{figure}$	Figure 11: Panel a): C/M foreground corrected versus galactocentric distance; Panel b): corresponding [Fe/H] radial gradient (see text).
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