All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1850f1.ps} \end{figure}$ Figure 1: The distribution of completeness, the fraction of targeted galaxies to all galaxies ( upper panel), and efficiency, the fraction of spectra that yielded a redshift determination ( lower panel) per field.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f2.ps} \end{figure}$ Figure 2: The completeness ( upper panel) and efficiency ( lower panel) as function of magnitude as found for the cluster EISJ0953-2017. The completeness and efficiency for this cluster as computed in Table 2 correspond to the typical values as can be seen in Fig. 1.
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In the text

$\begin{figure} \par\resizebox{4.2cm}{!}{\includegraphics{1850f3a.ps}}\resizebox{... ...izebox{4.2cm}{!}{\includegraphics{1850f3u.ps}}\hspace*{6.7cm}}\par\end{figure}$ Figure 3: Redshift distributions for the 21 observed cluster fields. Note that the scale of the y-axis differs between the panels. The upper panels show bar diagrams of the measured redshifts, while the lower panels give the corresponding histograms of the redshift distributions (dotted line). The solid lines mark the detected groups.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1850f4a.ps} \end{figure}$ Figure 4: Projected distributions of $I\leq 19.5$ galaxies (small symbols) in each of the cluster fields. The number on the left-hand side refers to Table 5. The matched filter center of the cluster is in the center of the plots. The dashed line marks the region covered by the MOS-masks. In some cases the MOS-masks are not centered on the cluster center due to the distribution of the bright galaxies. The filled circles mark spectroscopic members of the confirmed systems, and the crosses galaxies with redshifts not belonging to the group. The large circles indicate a region of $0.5~h_{75}^{-1}~{\rm Mpc}$ at the redshift of the confirmed group.
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In the text

$\begin{figure}\par\includegraphics[width=16.4cm,clip]{1850f4b.ps}\end{figure}$ Figure 4: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f5.ps} \end{figure}$ Figure 5: The distribution of spectroscopic redshifts of all the confirmed systems.
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In the text

$\begin{figure} \par\resizebox{3.7cm}{!}{\includegraphics{1850f6a.ps}}\resizebox{... ...cs{1850f6zf.ps}}\resizebox{3.7cm}{!}{\includegraphics{1850f6zg.ps}} \end{figure}$ Figure 6: Detailed redshift diagrams for all spectroscopically confirmed systems. The identification numbers in each panel refer to Table 5. Upper panels show a bar diagram of the redshifts of cluster members. The lower part shows the redshift histogram with a bin size of $\Delta z=0.002$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f7.ps} \end{figure}$ Figure 7: Distribution of velocity dispersions (solid line) compared with those of Fadda et al. (1996) - dotted histogram - and those of Zabludoff et al. (1990) - triple dot-dashed histogram.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f8.ps} \end{figure}$ Figure 8: The relation between the original matched filter estimated $\Lambda _{\rm cl, org}$ richnesses and the new ones, $\Lambda _{\rm cl, new}$ . The solid line marks $\Lambda _{\rm cl, org}=\Lambda _{\rm cl, new}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f9.ps} \end{figure}$ Figure 9: The distribution of $\Lambda _{\rm cl, new}$ -richnesses.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f10.ps} \end{figure}$ Figure 10: The distribution of concentration indices for the confirmed systems (solid line) compared with the distribution from Butcher & Oemler (1984) given by the dashed histogram.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f12.ps} \end{figure}$ Figure 12: Distribution of red sequence S/N values for 1000 random galaxy samples for three different redshifts.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f13.ps} \end{figure}$ Figure 13: Distribution of the measured scatter around the red sequences (solid line) compared to that of López-Cruz et al. (2004) (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f14.ps} \end{figure}$ Figure 14: The relation between $\Lambda _{\rm cl, new}$ and $\sigma _{\rm v}$ for the 31 confirmed systems with a measured velocity dispersion. The solid line marks the scaling relation derived by Bahcall et al. (2003) with the dashed lines marking its uncertainty.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f15.ps} \end{figure}$ Figure 15: The colour dispersion as function of redshift for all systems with a red sequence identified in the spectroscopic analysis.
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In the text

$\begin{figure} \par\resizebox{5.5cm}{!}{\includegraphics{1850f16a.ps}}\resizebox... ...cs{1850f16b.ps}}\resizebox{5.5cm}{!}{\includegraphics{1850f16c.ps}} \end{figure}$ Figure 16: Global properties of the red-sequence systems (gray region) compared with those of the entire sample (solid line). The left panel shows the distribution of velocity dispersion, the middle panel that of richness and the right panel that of concentration index.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f17.ps} \end{figure}$ Figure 17: The relation between $\Lambda _{\rm cl, new}$ and $\sigma _{\rm v}$ for the 17 systems for which we identify red sequences from the spectrocopic analysis. The solid line marks the scaling relation derived by Bahcall et al. (2003) with the dashed lines marking its uncertainty.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f18.ps} \end{figure}$ Figure 18: The relation between the redshift of the systems and the colour of the red sequence. The number 2 indicates that there are two symbols falling almost on top of each other. The lines mark the no-evolution (thin line) and the passive evolution (thick line) predictions.
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In the text

$\begin{figure} \par\resizebox{5cm}{!}{\includegraphics{185011a1.ps}}\resizebox{5... ...{185011e2.ps}}\resizebox{5cm}{!}{\includegraphics{185011e3.ps}}\par \end{figure}$ Figure 11: For each cluster we show 3 diagrams with the cluster identification number indicated in the first one. The first diagram is the colour-magnitude diagram for all galaxies within $0.75~h_{75}^{-1}~{\rm Mpc}$ from the cluster center (dots). On top of that we mark by solid circles the spectroscopic members of the confirmed group and by crosses the remaining galaxies with redshifts. The solid line is the locus of the red sequence detected from the spectroscopic members and the dashed line is the one detected in the photometric analysis. In both cases we only show the line if we consider the sequence significant (see the text for details). The second plot is the "tilted colour histogram'' for the galaxies with $I\leq 19.5$ in the same region statistically corrected for the background contribution. The last panel is the "tilted colour histogram'' for the spectroscopic members (solid line) and for all galaxies with a redshift (dotted line).
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In the text

$\begin{figure}\par\resizebox{5cm}{!}{\includegraphics{185011f1.ps}}\resizebox{5c... ...s{185011k2.ps}}\resizebox{5cm}{!}{\includegraphics{185011k3.ps}}\par\end{figure}$ Figure 11: continued.
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In the text

$\begin{figure}\par\resizebox{5cm}{!}{\includegraphics{185011l1.ps}}\resizebox{5c... ...s{185011q2.ps}}\resizebox{5cm}{!}{\includegraphics{185011q3.ps}}\par\end{figure}$ Figure 11: continued.
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In the text

$\begin{figure}\par\resizebox{5cm}{!}{\includegraphics{185011r1.ps}}\resizebox{5c... ...s{185011w2.ps}}\resizebox{5cm}{!}{\includegraphics{185011w3.ps}}\par\end{figure}$ Figure 11: continued.
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In the text

$\begin{figure}\par\resizebox{5cm}{!}{\includegraphics{185011x1.ps}}\resizebox{5c... ...s{18501132.ps}}\resizebox{5cm}{!}{\includegraphics{18501133.ps}}\par\end{figure}$ Figure 11: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1850f1.ps} \end{figure}$	Figure 1: The distribution of completeness, the fraction of targeted galaxies to all galaxies ( upper panel), and efficiency, the fraction of spectra that yielded a redshift determination ( lower panel) per field.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f2.ps} \end{figure}$	Figure 2: The completeness ( upper panel) and efficiency ( lower panel) as function of magnitude as found for the cluster EISJ0953-2017. The completeness and efficiency for this cluster as computed in Table 2 correspond to the typical values as can be seen in Fig. 1.
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$\begin{figure} \par\resizebox{4.2cm}{!}{\includegraphics{1850f3a.ps}}\resizebox{... ...izebox{4.2cm}{!}{\includegraphics{1850f3u.ps}}\hspace*{6.7cm}}\par\end{figure}$	Figure 3: Redshift distributions for the 21 observed cluster fields. Note that the scale of the y-axis differs between the panels. The upper panels show bar diagrams of the measured redshifts, while the lower panels give the corresponding histograms of the redshift distributions (dotted line). The solid lines mark the detected groups.
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$\begin{figure}\par\includegraphics[width=16.4cm,clip]{1850f4b.ps}\end{figure}$	Figure 4: continued.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f5.ps} \end{figure}$	Figure 5: The distribution of spectroscopic redshifts of all the confirmed systems.
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$\begin{figure} \par\resizebox{3.7cm}{!}{\includegraphics{1850f6a.ps}}\resizebox{... ...cs{1850f6zf.ps}}\resizebox{3.7cm}{!}{\includegraphics{1850f6zg.ps}} \end{figure}$	Figure 6: Detailed redshift diagrams for all spectroscopically confirmed systems. The identification numbers in each panel refer to Table 5. Upper panels show a bar diagram of the redshifts of cluster members. The lower part shows the redshift histogram with a bin size of $\Delta z=0.002$ .
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f7.ps} \end{figure}$	Figure 7: Distribution of velocity dispersions (solid line) compared with those of Fadda et al. (1996) - dotted histogram - and those of Zabludoff et al. (1990) - triple dot-dashed histogram.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f8.ps} \end{figure}$	Figure 8: The relation between the original matched filter estimated $\Lambda _{\rm cl, org}$ richnesses and the new ones, $\Lambda _{\rm cl, new}$ . The solid line marks $\Lambda _{\rm cl, org}=\Lambda _{\rm cl, new}$ .
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f9.ps} \end{figure}$	Figure 9: The distribution of $\Lambda _{\rm cl, new}$ -richnesses.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f10.ps} \end{figure}$	Figure 10: The distribution of concentration indices for the confirmed systems (solid line) compared with the distribution from Butcher & Oemler (1984) given by the dashed histogram.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f12.ps} \end{figure}$	Figure 12: Distribution of red sequence S/N values for 1000 random galaxy samples for three different redshifts.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f13.ps} \end{figure}$	Figure 13: Distribution of the measured scatter around the red sequences (solid line) compared to that of López-Cruz et al. (2004) (dashed line).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f14.ps} \end{figure}$	Figure 14: The relation between $\Lambda _{\rm cl, new}$ and $\sigma _{\rm v}$ for the 31 confirmed systems with a measured velocity dispersion. The solid line marks the scaling relation derived by Bahcall et al. (2003) with the dashed lines marking its uncertainty.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{1850f15.ps} \end{figure}$	Figure 15: The colour dispersion as function of redshift for all systems with a red sequence identified in the spectroscopic analysis.
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$\begin{figure} \par\resizebox{5.5cm}{!}{\includegraphics{1850f16a.ps}}\resizebox... ...cs{1850f16b.ps}}\resizebox{5.5cm}{!}{\includegraphics{1850f16c.ps}} \end{figure}$	Figure 16: Global properties of the red-sequence systems (gray region) compared with those of the entire sample (solid line). The left panel shows the distribution of velocity dispersion, the middle panel that of richness and the right panel that of concentration index.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f17.ps} \end{figure}$	Figure 17: The relation between $\Lambda _{\rm cl, new}$ and $\sigma _{\rm v}$ for the 17 systems for which we identify red sequences from the spectrocopic analysis. The solid line marks the scaling relation derived by Bahcall et al. (2003) with the dashed lines marking its uncertainty.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1850f18.ps} \end{figure}$	Figure 18: The relation between the redshift of the systems and the colour of the red sequence. The number 2 indicates that there are two symbols falling almost on top of each other. The lines mark the no-evolution (thin line) and the passive evolution (thick line) predictions.
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$\begin{figure}\par\resizebox{5cm}{!}{\includegraphics{185011f1.ps}}\resizebox{5c... ...s{185011k2.ps}}\resizebox{5cm}{!}{\includegraphics{185011k3.ps}}\par\end{figure}$	Figure 11: continued.
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