All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig1.ps}}\end{figure}$ Figure 1: Redshift distribution of the cluster sample used in this paper.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig2.ps}}\end{figure}$ Figure 2: Relation between the optical luminosity calculated in the SDSS r band within r₂₀₀ and the number of cluster galaxies contributing to $L_{\rm op}$ . The solid line is the best fit line with slope $1.00\pm 0.03$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig3.ps}}\end{figure}$ Figure 3: The stacked mean surface number density profile of all the cluster galaxies with magnitude r < -18.5. The solid curve is the best fit King profile, the dashed curve is the best fit NFW profile.
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In the text

$\begin{figure} \par\resizebox{14.3cm}{!}{\includegraphics{4708fig4.ps}}\end{figure}$ Figure 4: The stacked surface number density profiles of clusters in different cluster mass bins. The individual cluster profiles are obtained by considering all the galaxies with $r_{\rm petro} < -18.5$ . The dashed curve in each panel is the King profile that provides the best-fit to the surface density profile shown in that same panel, while the solid curve is the King profile that provides the best-fit to the mean stacked surface density profile (same as the solid line in Fig. 3). The dotted line in the bottom panels (corresponding to the highest-mass bin clusters) is the best fit provided by a generalized King profile.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig5.ps}}\end{figure}$ Figure 5: The surface number density profile of all the cluster galaxies with r < -18.5 in the highest of our considered cluster mass bins. The solid curve is the best fit provided by the generalized King profile. The dashed curve is the best fit provided by the NFW profile. Both profiles are consistent with the data.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig6.ps}}\end{figure}$ Figure 6: Composite surface brightness profile of two cluster samples: the low mass systems at $M_{200} \le 10^{14} ~M_{\odot}$ (empty squares) and the massive clusters at $M_{200} > 3\times 10^{15}~ M_{\odot}$ (filled dots).
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In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics{4708fig7.ps}}\end{figure}$ Figure 7: The stacked surface number density profile of the red cluster galaxies with magnitude r < -18.5, separately for clusters of different masses. The meaning of the lines is the same as in Fig. 4.
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In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics{4708fig8.ps}}\end{figure}$ Figure 8: The stacked surface number density profile of the blue cluster galaxies with magnitude r < -18.5, separately for clusters of different masses. The meaning of the lines is the same as in Fig. 4.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig9.ps}}\end{figure}$ Figure 9: $L_{\rm op}{-}M_{200}$ relation. The optical luminosity is calculated within r₂₀₀ and is corrected for contamination due to projection effect. The empty squares in the plot are the X-ray selected clusters. The filled points are the optically selected clusters. The solid line in the plot is the best fit line of the corrected $L_{\rm op}{-}M_{200}$ relation. The dashed line is the best fit line of the uncorrected $L_{\rm op}{-}M_{200}$ relation.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig10.eps}}\end{figure}$ Figure 10: $N_{\rm gal}{-}M_{200}$ relation. The number of cluster galaxies is calculated within r₂₀₀ and is corrected for contamination due to projection effect. The empty squares in the plot are the X-ray selected clusters. The filled points are the optically selected clusters. The solid line in the plot is the best fit line of the corrected $N_{\rm gal}{-}M_{200}$ relation. The dashed line is the best fit line of the uncorrected $N_{\rm gal}{-}M_{200}$ relation.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig11.ps}}\end{figure}$ Figure 11: Relation between the i band Petrosian absolute magnitude and the galaxy stellar mass. The galaxy stellar masses are taken by Kauffmann et al. (2003).
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In the text

$\begin{figure} \par\mbox{\resizebox{8.8cm}{!}{\includegraphics{4708fig12.ps}}\resizebox{8.8cm}{!}{\includegraphics{4708fig13.ps}} } \end{figure}$ Figure 12: The composite LF for the whole ( left panel) and the red ( right panel) cluster galaxy populations. In both panels the filled points are the low-mass clusters ( $M_{200}/10^{14}~M_{\odot} \le 1$ ), the empty squares the intermediate-mass systems ( $1 \le M_{200}/10^{14}~M_{\odot} \le 10$ ) and the empty triangles are the high-mass clusters ( $M_{200}/10^{14}~M_{\odot} \ge 10$ ). The different mass-bin LFs are renormalized so as to ease the comparisons among them. The solid lines in the panels are the best fits obtained in Popesso et al. (2006) from the X-ray selected RASS-SDSS galaxy clusters for the corresponding whole and red cluster galaxy populations.
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In the text

$\begin{figure*} \par\resizebox{7cm}{!}{\includegraphics{4708fig14.ps}}\par\resiz... ...708fig15.ps}}\par\resizebox{7cm}{!}{\includegraphics{4708fig16.ps}}\end{figure*}$ Figure 13: Upper panel: the magnitude of the BCGs (empty squares) within r₂₀₀ as a function of the number of cluster galaxies within the same radius, and with $r \le -18.5$ mag. The solid line in the plot shows the expected BCG magnitude as estimated from the best-fitting composite LF, as a function of the cluster normalization. The dashed lines are the statistical uncertainties in the relation represented by the solid line. The filled squares are the median magnitudes per bin of $N_{{\rm gal}}$ . Middle panel: same as the left panel, but for the second brightest cluster galaxies. Bottom panel: same as the left panel, but for the third brightest cluster galaxies.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig17.ps}}\end{figure}$ Figure 14: The relation between BCG luminosity and cluster mass for our cluster sample. Cluster masses are computed from $N_{{\rm gal}}$ s using our derived HOD. The solid line in the plot is the best-fit line obtained with an orthogonal linear regression, $L_{\rm BCG} \propto M_{200}^{0.33\pm 0.04}$ , and the dashed line is Lin & Mohr's (2004) relation. Other symbols have the same meaning as in the Fig. 13.
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In the text

$\begin{figure} \par\mbox{\resizebox{8.8cm}{!}{\includegraphics{4708fig18.ps}}\resizebox{8.8cm}{!}{\includegraphics{4708fig19.ps}} } \end{figure}$ Figure 15: Left panel: the best-fit FP of cluster ellipticals, relating their internal velocity dispersions ( $\sigma$ ), effective radii ( $r_{\rm e}$ ), and surface brightnesses within $r_{\rm e}$ ( $\mu$ ). The different symbols in the plot indicate elliptical galaxies of clusters in different mass bins. The right-hand side panel shows the mean residuals from the global FP of the elliptical populations of individual clusters as a function of the cluster mass.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig1.ps}}\end{figure}$	Figure 1: Redshift distribution of the cluster sample used in this paper.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig2.ps}}\end{figure}$	Figure 2: Relation between the optical luminosity calculated in the SDSS r band within r₂₀₀ and the number of cluster galaxies contributing to $L_{\rm op}$ . The solid line is the best fit line with slope $1.00\pm 0.03$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig3.ps}}\end{figure}$	Figure 3: The stacked mean surface number density profile of all the cluster galaxies with magnitude r < -18.5. The solid curve is the best fit King profile, the dashed curve is the best fit NFW profile.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig5.ps}}\end{figure}$	Figure 5: The surface number density profile of all the cluster galaxies with r < -18.5 in the highest of our considered cluster mass bins. The solid curve is the best fit provided by the generalized King profile. The dashed curve is the best fit provided by the NFW profile. Both profiles are consistent with the data.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig6.ps}}\end{figure}$	Figure 6: Composite surface brightness profile of two cluster samples: the low mass systems at $M_{200} \le 10^{14} ~M_{\odot}$ (empty squares) and the massive clusters at $M_{200} > 3\times 10^{15}~ M_{\odot}$ (filled dots).
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$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics{4708fig7.ps}}\end{figure}$	Figure 7: The stacked surface number density profile of the red cluster galaxies with magnitude r < -18.5, separately for clusters of different masses. The meaning of the lines is the same as in Fig. 4.
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$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics{4708fig8.ps}}\end{figure}$	Figure 8: The stacked surface number density profile of the blue cluster galaxies with magnitude r < -18.5, separately for clusters of different masses. The meaning of the lines is the same as in Fig. 4.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4708fig11.ps}}\end{figure}$	Figure 11: Relation between the i band Petrosian absolute magnitude and the galaxy stellar mass. The galaxy stellar masses are taken by Kauffmann et al. (2003).
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