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All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f1.eps} \end{figure}$ Figure 1: Completeness magnitudes of the B- and R-band images, as estimated by comparing the magnitudes in the fixed aperture ( $m_{\rm ap}$ ) and in the detection cell ( $m_{\rm cell}$ ). The horizontal solid lines represent the completeness limits, the vertical dot-dashed lines mark the limits in the detection cell, and the dashed lines are the linear relations between $m_{\rm ap}$ and $m_{\rm cell}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{0841_f2.eps} \end{figure}$ Figure 2: Photometric properties of sources classified by SExtractor as being stars. ( Top panel) Number-magnitude distribution of stars. The best-fitting power-law function to the counts for 19<R<22 is indicated, as is the R=23 magnitude limit used for analysis of the red sequence galaxy population. ( Bottom panel) B-R colour distribution of 19<R<22 stars, normalised to match the expected level of stellar contamination for 22<R<23.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{0841_f3.eps} \end{figure}$ Figure 3: The surface density of R<23.0 galaxies in the field of A 209. The dashed contour corresponds to the field galaxy number density, while the solid contours correspond respectively to 2, 3.3, 5, 7.5, 10, and 12.5 cluster galaxies arcmin^-2. The shaded boxes indicate the regions used to represent the field galaxy population.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f4.eps} \end{figure}$ Figure 4: The B-R/R colour-magnitude diagrams of the cluster galaxy population in the three cluster regions corresponding to high-, intermediate-, and low-density environments. Each of the three diagrams is the result of a Monte-Carlo realisation in which field galaxies are subtracted statistically. For comparison the C-M diagram of field galaxies is shown also. In each plot the solid line indicates the best-fitting C-M relation of Eq. (4), and galaxies identified as belonging to the red sequence through Eq. (6) are indicated by solid circles.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f5.eps} \end{figure}$ Figure 5: The B- and R-band LFs of galaxies in the virial region. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in Table 2. In the small panels, the 1, 2 and $3\sigma$ confidence levels of the best-fitting parameters $\alpha$ and M^* are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0841_f6.eps} \end{figure}$ Figure 6: The B-band LFs of galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0841_f7.eps} \end{figure}$ Figure 7: The 1, 2 and $3\sigma$ confidence limits for the best-fitting Schechter parameters $\alpha$ and B^* for the three cluster regions corresponding to low- (solid contours), intermediate- (dotted) and high-density (dashed) environments.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{0841_f8.eps} \end{figure}$ Figure 8: The R-band LFs of galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0841_f9.eps} \end{figure}$ Figure 9: Confidence limits for the best-fitting Schechter parameters $\alpha$ and R^* for the three cluster regions. Contours as for Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f10.eps} \end{figure}$ Figure 10: The R-band LF of red sequence galaxies in the virial region. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in the top-left of each plot. In the small panels, the 1, 2 and $3\sigma$ confidence levels of the best-fitting parameters $\alpha$ and R^* are shown.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0841_f11.eps} \end{figure}$ Figure 11: The R-band LFs of red sequence galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in the top-left of each plot.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{0841_f12.eps} \end{figure}$ Figure 12: Confidence limits for the best-fitting Schechter parameters $\alpha$ and R^* for the three cluster regions. Contours as for Fig. 7.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f13.eps} \end{figure}$ Figure 13: The blue galaxy fraction as a function of local number density.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f14.eps} \end{figure}$ Figure 14: The mean galaxy colour of the cluster galaxy population as a function of spatial position (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{0841_f3.eps} \end{figure}$	Figure 3: The surface density of R<23.0 galaxies in the field of A 209. The dashed contour corresponds to the field galaxy number density, while the solid contours correspond respectively to 2, 3.3, 5, 7.5, 10, and 12.5 cluster galaxies arcmin^-2. The shaded boxes indicate the regions used to represent the field galaxy population.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f5.eps} \end{figure}$	Figure 5: The B- and R-band LFs of galaxies in the virial region. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in Table 2. In the small panels, the 1, 2 and $3\sigma$ confidence levels of the best-fitting parameters $\alpha$ and M^* are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0841_f6.eps} \end{figure}$	Figure 6: The B-band LFs of galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0841_f7.eps} \end{figure}$	Figure 7: The 1, 2 and $3\sigma$ confidence limits for the best-fitting Schechter parameters $\alpha$ and B^* for the three cluster regions corresponding to low- (solid contours), intermediate- (dotted) and high-density (dashed) environments.
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$\begin{figure} \includegraphics[angle=-90,width=8.8cm,clip]{0841_f8.eps} \end{figure}$	Figure 8: The R-band LFs of galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0841_f9.eps} \end{figure}$	Figure 9: Confidence limits for the best-fitting Schechter parameters $\alpha$ and R^* for the three cluster regions. Contours as for Fig. 7.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f10.eps} \end{figure}$	Figure 10: The R-band LF of red sequence galaxies in the virial region. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in the top-left of each plot. In the small panels, the 1, 2 and $3\sigma$ confidence levels of the best-fitting parameters $\alpha$ and R^* are shown.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{0841_f11.eps} \end{figure}$	Figure 11: The R-band LFs of red sequence galaxies in the three cluster regions corresponding to high-, intermediate- and low-density environments. The solid curve indicates the best-fitting Schechter function whose parameters are indicated in the top-left of each plot.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{0841_f12.eps} \end{figure}$	Figure 12: Confidence limits for the best-fitting Schechter parameters $\alpha$ and R^* for the three cluster regions. Contours as for Fig. 7.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f13.eps} \end{figure}$	Figure 13: The blue galaxy fraction as a function of local number density.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0841_f14.eps} \end{figure}$	Figure 14: The mean galaxy colour of the cluster galaxy population as a function of spatial position (see text).
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