All Figures

$\begin{figure} \par\includegraphics[width=5cm,clip]{9600fig1.ps}\end{figure}$ Figure 1: Absolute magnitude histogram of the galaxies in the five clusters. The dotted line shows the completeness magnitude limit for each cluster; the dashed line shows the common magnitude limit we have adopted for the five clusters.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9600fig2.ps}\end{figure}$ Figure 2: Left panels: the color-magnitude diagrams for the five clusters. The solid line is the fit to the red sequence and the dotted line is the upper 0.2 mag limit. The vertical line corresponds to the limit M_r = -20 at the cluster redshift. Right panels: the histograms of the B-r distance of the galaxies to the corresponding red sequence.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{9600fig3.ps}\end{figure}$ Figure 3: Slopes of the CMR for the sample of López-Cruz et al. (2004) (black circles) and our sample (empty triangles).
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In the text

$\begin{figure} \par\includegraphics[clip,width=0.8\hsize]{9600fig4.ps}\par\includegraphics[clip,width=0.8\hsize]{9600fig5.ps}\end{figure}$ Figure 4: Blue fraction of galaxies in our sample of clusters (triangles) compared with those obtained by De Propris et al. (2004) (black circles) for an aperture of r₂₀₀/2. The top (bottom) panel corresponds to the blue fraction computed within a radius of 420 kpc (735 kpc).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{9600fig6.ps}\end{figure}$ Figure 5: The visual classification differences between Fasano et al. (2000) and this paper.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{9600fig7.ps}\end{figure}$ Figure 6: Cumulative functions of the different morphological types as a function of the projected radius to the center of the cluster. Early types: solid lines; late types: dotted lines. The vertical lines indicate the radius where the distributions reach the 50% level.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9600fig8.ps}\end{figure}$ Figure 7: Concentration parameter versus redshift for our clusters (triangles), a low-redshift compilation (Butcher & Oemler 1978: black points) and a higher redshift sample (Dressler et al. 1997: asteriks). The horizontal line is the mean concentration value of the clusters with enough area coverage.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9600fig9.ps}\end{figure}$ Figure 8: Histogram of the f-parameter values for the galaxies belonging to our clusters.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{9600fig1.ps}\end{figure}$	Figure 1: Absolute magnitude histogram of the galaxies in the five clusters. The dotted line shows the completeness magnitude limit for each cluster; the dashed line shows the common magnitude limit we have adopted for the five clusters.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9600fig2.ps}\end{figure}$	Figure 2: Left panels: the color-magnitude diagrams for the five clusters. The solid line is the fit to the red sequence and the dotted line is the upper 0.2 mag limit. The vertical line corresponds to the limit M_r = -20 at the cluster redshift. Right panels: the histograms of the B-r distance of the galaxies to the corresponding red sequence.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{9600fig3.ps}\end{figure}$	Figure 3: Slopes of the CMR for the sample of López-Cruz et al. (2004) (black circles) and our sample (empty triangles).
Open with DEXTER

$\begin{figure} \par\includegraphics[clip,width=0.8\hsize]{9600fig4.ps}\par\includegraphics[clip,width=0.8\hsize]{9600fig5.ps}\end{figure}$	Figure 4: Blue fraction of galaxies in our sample of clusters (triangles) compared with those obtained by De Propris et al. (2004) (black circles) for an aperture of r₂₀₀/2. The top (bottom) panel corresponds to the blue fraction computed within a radius of 420 kpc (735 kpc).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{9600fig6.ps}\end{figure}$	Figure 5: The visual classification differences between Fasano et al. (2000) and this paper.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm,clip]{9600fig7.ps}\end{figure}$	Figure 6: Cumulative functions of the different morphological types as a function of the projected radius to the center of the cluster. Early types: solid lines; late types: dotted lines. The vertical lines indicate the radius where the distributions reach the 50% level.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9600fig8.ps}\end{figure}$	Figure 7: Concentration parameter versus redshift for our clusters (triangles), a low-redshift compilation (Butcher & Oemler 1978: black points) and a higher redshift sample (Dressler et al. 1997: asteriks). The horizontal line is the mean concentration value of the clusters with enough area coverage.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9600fig9.ps}\end{figure}$	Figure 8: Histogram of the f-parameter values for the galaxies belonging to our clusters.
Open with DEXTER