All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F01.ps} \end{figure}$ Figure 1: Area covered by the photometry in the region of ABCG 209. All the galaxies brighter than V = 21.5 are marked with crosses. The central field (solid contour) was observed in B, V and R bands, while the two adjacent fields (dashed contours) were observed only in V band. Circles mark the regions analysed in Sect. 6.1. North is up and East is on the left. The origin of the coordinates coincides with the cluster center ( $\alpha _{2000} = 01$ 31 52.7, $\delta _{2000} = -13$ 36 41.9). A region around a bright star was not considered in the analysis (right bottom corner of central field).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F02.ps} \end{figure}$ Figure 2: Completeness magnitudes of the B-, V-, and R-band images are estimated by comparing magnitudes in the fixed aperture ( $M_{{\rm ap}}$ ) and in the detection cell ( $M_{{\rm cell}}$ ). The dotted lines represent the completeness limits, the dashed lines mark the limits in the detection cell, and solid lines are the linear relations between $M_{{\rm ap}}$ and $M_{{\rm cell}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F03.ps} \end{figure}$ Figure 3: Luminosity function in the B, V and R bands in the central field of $9.2^\prime \times 8.6^\prime$ . In V and R bands filled circles represent counts obtained from the photometric catalog with a statistical background subtraction, open circles are the counts of galaxies belonging to the red sequence of the CM relation (see Sect. 5.2). Solid and dashed lines are the Schechter fits to the filled and open circles respectively. In the small panels the 1, 2 and 3 $\sigma$ c.l. of the best-fit parameters $\alpha$ and M^* are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F04.ps} \end{figure}$ Figure 4: Luminosity function in the V and R bands in the central field of $9.2^\prime \times 8.6^\prime$ . The dashed lines represent the Schechter functions for bright and faint galaxies separately (see text). The continuous line represents the sum of the two functions. In the small panels the 1, 2 and 3 $\sigma$ c.l. of the best-fit parameters $\alpha$ and M^* are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F05.ps} \end{figure}$ Figure 5: V-R vs. R CM diagram for all the galaxies within the completeness limit in the central field of ABCG 209. Galaxies of the red sequence (see solid line) are plotted as filled circles. The solid line defines the CM sequence for spectroscopically confirmed cluster members.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F06.ps} \end{figure}$ Figure 6: Luminosity function in the V band. In the upper panel are shown the LF in the whole observed area (160 arcmin²) and the 1, 2 and 3 $\sigma$ c.l. of the best-fit parameters $\alpha$ and M^* (small panel). The continuous line represents the fitted Schechter functions. In the other panels the LFs in the three cluster regions (see text) are shown. Continuous lines are the fit of the Schechter functions obtained by fixing the faint-end slope at the best fit value of the LF fitted on the whole observed area.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,height=14.5cm,angle=-90]{H4349F07.ps} \end{figure}$ Figure 7: Background-subtracted radial profile of ABCG 209 is shown in the left panel. Open circles represent the distribution of all galaxies in the cluster, filled circles are bright galaxies ( $M{^*_V \le } -19.5$ ) and open triangles are faint galaxies ( M^*_V > -19.5). The number of bright galaxies in the first and in the second bin is $\sim$ 32 and $\sim$ 17 respectively, while the number of faint galaxies is $\sim$ 15 and $\sim$ 30. The bright-to-faint ratio as a function of the clustercentric distance is shown in the right panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F02.ps} \end{figure}$	Figure 2: Completeness magnitudes of the B-, V-, and R-band images are estimated by comparing magnitudes in the fixed aperture ( $M_{{\rm ap}}$ ) and in the detection cell ( $M_{{\rm cell}}$ ). The dotted lines represent the completeness limits, the dashed lines mark the limits in the detection cell, and solid lines are the linear relations between $M_{{\rm ap}}$ and $M_{{\rm cell}}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F04.ps} \end{figure}$	Figure 4: Luminosity function in the V and R bands in the central field of $9.2^\prime \times 8.6^\prime$ . The dashed lines represent the Schechter functions for bright and faint galaxies separately (see text). The continuous line represents the sum of the two functions. In the small panels the 1, 2 and 3 $\sigma$ c.l. of the best-fit parameters $\alpha$ and M^* are shown.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4349F05.ps} \end{figure}$	Figure 5: V-R vs. R CM diagram for all the galaxies within the completeness limit in the central field of ABCG 209. Galaxies of the red sequence (see solid line) are plotted as filled circles. The solid line defines the CM sequence for spectroscopically confirmed cluster members.
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