All Figures

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-f1a.eps}} \resizebox{\hsize}{!}{\includegraphics[clip]{3413-f1b.eps}} \end{figure}$ Figure 1: i-band CCD images of the two M 31 companions NGC 185 (upper) and NGC 147 (lower), obtained at the 2.56 m Nordic Optical Telescope. The field covers ${\approx }6\hbox {$.\mkern -4mu^\prime $ }5\times 6\hbox {$.\mkern -4mu^\prime $ }5$ , i.e. most of the galaxies. North is up and east is to the left. The seeing is $\approx$ 0.7 $^{\prime \prime }$ and 1 $^{\prime \prime }$ , respectively. In the lower left foreground of NGC 147, the minor planet 2000 PT₂₇ can be seen, which was discovered only 3 weeks before our observations (Nowotny & Karlsson 2000).
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{3413-fig2.eps} \end{figure}$ Figure 2: Colour-magnitude diagrams for all stars having good photometry in V and i (sample 1; mean 1 $\sigma$ error bars are given for different i₀ magnitude ranges). Triangles mark the RGB-tips, as we determined it in Sect. 4.1. The absolute magnitudes are calculated using the distance moduli from Table 1.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig3.eps}} \end{figure}$ Figure 3: i₀-LF for all stars of sample 1 for both galaxies. Overplotted is the resulting histogram of the edge-detection algorithm (zero-sum Sobel kernel), from which we calculated the magnitude of the RGB-tip.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{3413-fig4.eps} \end{figure}$ Figure 4: Left: colour-colour diagrams for all stars of sample 2. Also plotted are the selection areas for M and C stars, as described in the text. Right: corresponding colour-magnitude diagrams for all stars of sample 2. The identified C stars from the selection areas, marked with open circles, lie on the uppermost parts of the RGB/AGB-sequences.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{3413-fig5.eps} \end{figure}$ Figure 5: Left: luminosity function (apparent and absolute i magnitude) for all C stars, identified in Fig. 4, of NGC 185 and NGC 147. Using the distance moduli from Table 1, one can calculate a $\langle$ M_i $\rangle$ (upper right corner). The dotted line marks the RGB-tip from Sect. 4.1. Right: bolometric LFs for all C stars found in NGC 185 and NGC 147. $M_{\rm bol}$ was calculated as described in the text. Note the difference between the mean luminosity $\langle$ L $\rangle$ and the luminosity calculated from the mean $\langle$ $M_{\rm bol}$ $\rangle$ .
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig6.eps}} \end{figure}$ Figure 6: Distribution of all stars of sample 2 of NGC 185 (upper) and NGC 147 (lower) on the i-band frames, overplotted are the identified C stars and the galaxy centres (Sect. 3.3). One can see the effect of vignetting in the corners, the strips without stars at the lower ends are due to a shift of the telescope between observations of frames of different filters.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig7.eps}} \end{figure}$ Figure 7: Radial distributions of all stars of sample 2 and for the found C stars.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{3413-fig2.eps} \end{figure}$	Figure 2: Colour-magnitude diagrams for all stars having good photometry in V and i (sample 1; mean 1 $\sigma$ error bars are given for different i₀ magnitude ranges). Triangles mark the RGB-tips, as we determined it in Sect. 4.1. The absolute magnitudes are calculated using the distance moduli from Table 1.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig3.eps}} \end{figure}$	Figure 3: i₀-LF for all stars of sample 1 for both galaxies. Overplotted is the resulting histogram of the edge-detection algorithm (zero-sum Sobel kernel), from which we calculated the magnitude of the RGB-tip.
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$\begin{figure} \par\includegraphics[width=17.3cm,clip]{3413-fig4.eps} \end{figure}$	Figure 4: Left: colour-colour diagrams for all stars of sample 2. Also plotted are the selection areas for M and C stars, as described in the text. Right: corresponding colour-magnitude diagrams for all stars of sample 2. The identified C stars from the selection areas, marked with open circles, lie on the uppermost parts of the RGB/AGB-sequences.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig6.eps}} \end{figure}$	Figure 6: Distribution of all stars of sample 2 of NGC 185 (upper) and NGC 147 (lower) on the i-band frames, overplotted are the identified C stars and the galaxy centres (Sect. 3.3). One can see the effect of vignetting in the corners, the strips without stars at the lower ends are due to a shift of the telescope between observations of frames of different filters.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{3413-fig7.eps}} \end{figure}$	Figure 7: Radial distributions of all stars of sample 2 and for the found C stars.
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