All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{2954fig1.ps} \end{figure}$ Figure 1: The z-band DGR vs. the cluster mass (panel a)), the velocity dispersion $\sigma$ (panel b)), the X-ray luminosity (panel c)), and the optical luminosity (panel d)). The DGR is calculated within a circle of 1 Mpc radius centered on the X-ray cluster center. In each panel, we list the value of the Spearman's rank correlation coefficient and the implied probability of no correlation.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2954fig2.ps} \end{figure}$ Figure 2: The 4 panels show the composite LFs in the 4 Sloan bands. The individual LFs used to calculate the composite LFs are measured within the physical sizes of the clusters, as given by r₂₀₀.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2954fig3.ps} \end{figure}$ Figure 3: Contour plots of the 68%, 95%, and 99% confidence levels of the parameters of the bright-end component of the double-Schechter function fit to the 4 SDSS bands composite LFs. Solid (dotted) contours show the results for the composite LF computed within r₂₀₀(respectively r₅₀₀).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2954fig4.ps} \end{figure}$ Figure 4: Same as Fig. 3, but for the faint-end component.
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In the text

$\begin{figure} \parbox[]{10cm}{ \includegraphics[width=10cm,clip]{2954fig5.ps} }... ...par \vspace*{3mm} \includegraphics[width=4.5cm,clip]{2954fig7.ps}}\end{figure}$ Figure 5: Panel a): the individual r-band LFs within r₂₀₀ of a subsample of 15 clusters with the faintest absolute magnitude limit ( $M_{r,\rm lim}\le -15.5$ ). Empty squares and filled points distinguish the LFs computed from cluster members only (down to the SDSS spectroscopic completeness magnitude, $r \le 17.77$ ), and using a statistical background subtraction, respectively. The solid line is the composite LF. Cluster names are indicated. Panel b): the distribution of the $\chi ^2$ values obtained from the comparison of the composite and the 29 individual LFs of clusters with $M_{z,\rm lim} \ge -16.5$ mag. Panel c)): the z-band DGR distribution of the 29 clusters.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{2954fig8.ps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{2954fig9.ps} \end{figure}$ Figure 6: The z-band DGR within r₂₀₀ as a function of cluster mass (panel a)) and the cluster velocity dispersion (panel b)). If DGR is calculated within r₂₀₀ the anti-correlation with mass ( $\sigma$ , $L_{\rm X}$ and $L_{\rm op}$ ) disappears.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{2954fig10.ps}\hspace*{5mm} \includegraphics[width=7.6cm,clip]{2954fig11.ps} \end{figure}$ Figure 7: The background-subtracted u-r distribution of the galaxy members of the 15 clusters with the faintest absolute magnitude limit ( $M_{r, \rm lim} \ge -15$ ). a): Color distribution in the magnitude range $-18 \le M_r \le -16.5$ ; b): color distribution in the magnitude range $-16.5 \le M_r \le -15$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig12.ps} \end{figure}$ Figure 8: The LFs of 4 clusters computed as for Fig. 5 (filled points), and by additionally excluding all galaxies with $u-r \ge 3$ (empty squares).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig13.ps}\hspace*{2mm} \includegraphics[width=8cm,clip]{2954fig14.ps} \end{figure}$ Figure 9: The composite late-type and early-type LFs in four SDSS photometric bands. The late-type (early-type) LFs are displayed in the four panels on the left (respectively, right).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2954fig15.ps}\hspace*{3mm} \includegraphics[width=7.8cm,clip]{2954fig16.ps} \end{figure}$ Figure 10: The cluster LFs within different cluster apertures in the r band per morphological type. The increment of the apertures is $0.1\times r_{200}$ . The normalization of the fitting function is increasing at larger apertures. Panel a) shows the LF of the cluster red galaxy population, calculated within different clustercentric apertures expressed in unit of r₂₀₀. Panel b) shows the same for the cluster blue galaxy population. For simplicity we only plot the best fitting functions and not the data points.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig17.ps} \end{figure}$ Figure 11: The early-type LF calculated within three different cluster regions. Only the best fitting functions are plotted, for simplicity, and not the data points. The LFs are renormalized to the same value to emphasize the shape variations.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2954fig18.ps}\hspace*{2mm}... ...0.ps}\hspace*{2mm} \includegraphics[width=6.5cm,clip]{2954fig21.ps} \end{figure}$ Figure 12: The fraction of red and blue dwarf galaxies as a function of the cluster environments. Panel a) shows the cumulative radial profile of the fraction of blue (filled points) and red (empty squared) dwarf galaxies ( $-18 \le M_r \le -15$ mag). The fraction is defined on the total number of cluster dwarf galaxies in the considered magnitude range. Panel b) shows the differential radial profile of the ratio between red and blue dwarf galaxies. Panel c) shows the differential radial profile of the surface density of the bright cluster galaxies in clusters ( $M_r \le -18$ mag). Panel d) shows the relation between the surface density of bright galaxies and the fraction of red and blue dwarf galaxies calculated in the same clustercentric ring.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig22.ps} \end{figure}$ Figure 13: The density distribution of neighbors of late (dotted histogram) and early (solid histogram) galaxies in the field. We select a fairly complete sample of nearby galaxies ( $z\le 0.02$ ) from the Sloan spectroscopic sample in the magnitude region $-18 \le M_R \le -16$ . We calculate for each galaxy in the sample the local density of neighbor galaxies counting the number of systems with $M_R \le -18$ mag, within 2.5 Mpc projected radius and $\pm$ 500 km s^-1 of the galaxy position and redshift. The sample comprises 1561 systems.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2954fig1.ps} \end{figure}$	Figure 1: The z-band DGR vs. the cluster mass (panel a)), the velocity dispersion $\sigma$ (panel b)), the X-ray luminosity (panel c)), and the optical luminosity (panel d)). The DGR is calculated within a circle of 1 Mpc radius centered on the X-ray cluster center. In each panel, we list the value of the Spearman's rank correlation coefficient and the implied probability of no correlation.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2954fig2.ps} \end{figure}$	Figure 2: The 4 panels show the composite LFs in the 4 Sloan bands. The individual LFs used to calculate the composite LFs are measured within the physical sizes of the clusters, as given by r₂₀₀.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2954fig3.ps} \end{figure}$	Figure 3: Contour plots of the 68%, 95%, and 99% confidence levels of the parameters of the bright-end component of the double-Schechter function fit to the 4 SDSS bands composite LFs. Solid (dotted) contours show the results for the composite LF computed within r₂₀₀(respectively r₅₀₀).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2954fig4.ps} \end{figure}$	Figure 4: Same as Fig. 3, but for the faint-end component.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{2954fig8.ps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{2954fig9.ps} \end{figure}$	Figure 6: The z-band DGR within r₂₀₀ as a function of cluster mass (panel a)) and the cluster velocity dispersion (panel b)). If DGR is calculated within r₂₀₀ the anti-correlation with mass ( $\sigma$ , $L_{\rm X}$ and $L_{\rm op}$ ) disappears.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{2954fig10.ps}\hspace*{5mm} \includegraphics[width=7.6cm,clip]{2954fig11.ps} \end{figure}$	Figure 7: The background-subtracted u-r distribution of the galaxy members of the 15 clusters with the faintest absolute magnitude limit ( $M_{r, \rm lim} \ge -15$ ). a): Color distribution in the magnitude range $-18 \le M_r \le -16.5$ ; b): color distribution in the magnitude range $-16.5 \le M_r \le -15$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig12.ps} \end{figure}$	Figure 8: The LFs of 4 clusters computed as for Fig. 5 (filled points), and by additionally excluding all galaxies with $u-r \ge 3$ (empty squares).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig13.ps}\hspace*{2mm} \includegraphics[width=8cm,clip]{2954fig14.ps} \end{figure}$	Figure 9: The composite late-type and early-type LFs in four SDSS photometric bands. The late-type (early-type) LFs are displayed in the four panels on the left (respectively, right).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2954fig17.ps} \end{figure}$	Figure 11: The early-type LF calculated within three different cluster regions. Only the best fitting functions are plotted, for simplicity, and not the data points. The LFs are renormalized to the same value to emphasize the shape variations.
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