All Figures

$\begin{figure} \par\includegraphics[width=6cm,clip]{6830f1.eps}\end{figure}$ Figure 1: The distribution of overall completeness, the fraction of targeted galaxies to all galaxies ( upper panel), and overall efficiency, the fraction of spectra that yielded a redshift determination ( lower panel) per field. The overall completeness is defined for galaxies brighter than I=20.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6830f2.eps}\end{figure}$ Figure 2: The completeness ( upper panel) and efficiency ( lower panel) as function of magnitude as found for the clusters EISJ0049-2920 (#5, dotted line), a typical case of high efficiency, and EISJ2236-4026 (#7, dashed line), a typical case of low efficiency.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6830f3.eps}\end{figure}$ Figure 3: Redshift distributions for the observed cluster fields as indicated in each panel. 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 (dashed line). The solid lines mark the detected groups.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6830f4.eps}\end{figure}$ Figure 4: Image cutouts, centred at the original MF position and with a size of $\sim$ 4', and position plots for the ten fields with groups assigned to the EIS detection. In the image cutouts galaxies with I<21 are marked by circles and galaxies with redshifts and belonging to the group are indicated by diamonds. In the projected distributions all galaxies with $I\leq 20$ are indicated by the small dots, crosses mark galaxies with redshift and the member galaxies are marked by filled circles. The large circles centred on the MF position indicate a radius of 0.5 h₇₅^-1 Mpc. In cases where there are symbols of different size it relates to substructures in the redshift distribution. The dashed rectangle marks the region of the redshift survey and the dotted square outlines the area of the image cutout.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6830f5.eps}\end{figure}$ Figure 5: Image cutouts, centred at the original MF position and with a size of $\sim$ 4', and position plots for the nine fields with significant groups detected but not assigned to the EIS cluster candidate. In the image cutouts galaxies with I<21 are marked by circles and galaxies with redshifts are indicated by diamonds. In the field of EISJ2243-3942 the galaxy marked by the big square has a redshift of 0.2301. For EISJ2248-4015 the big squares mark four galaxies with redshifts in the range 0.2460-0.2484. In the projected distributions all galaxies with $I\leq 20$ are indicated by the small dots, crosses mark galaxies with redshift and each significant group is denoted by its own symbol. The dashed rectangle marks the region of the redshift survey and the dotted square outlines the area of the image cutout.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{6830f6.eps}\end{figure}$ Figure 6: Image cutouts for the four fields without significant groups detected. From left to right the panels show the field of EISJ0044-2950A, EISJ2241-4006, EISJ2243-4010A and EISJ2246-4012B. The cutouts are centred at the original position and have a size of $\sim$ 4 $\hbox {$^\prime $ }$ . Galaxies with I<21 are marked by circles, additional diamonds denote galaxies with measured redshifts. In the field of EISJ2243-4010A the galaxies marked by the big squares have redshifts in the range 0.3431-0.3471.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6830f7a.eps}\par\includegraphics[width=7cm,clip]{6830f7b.eps}\end{figure}$ Figure 7: Upper panel: the spectroscopic versus matched filter redshifts. Solid circles mark the confirmed systems, open circles mark systems from Paper III and triangles mark those systems that have a suggestive spectroscopic redshift. Lower panel: the distribution of the offset between the spectroscopic and matched-filter estimated redshifts of all the confirmed systems in this paper (solid line) and in Paper III (dashed line, scaled to match the same number of objects). The dotted histogram includes the two systems with a suggestive spectroscopic redshift.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6830f8.eps}\end{figure}$ Figure 8: Detailed redshift distributions for all systems considered confirmed.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6830f9.eps}\end{figure}$ Figure 9: Distribution of velocity dispersions (solid line) compared with that of the $z_{\rm MF}=0.2$ sample scaled to the same number of objects (dashed line, Paper III). The dotted histogram denote the distribution assuming that the four systems with substructure are superpositions and only the richest group is included as the confirmation.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{6830f10.eps}\end{figure}$ Figure 10: For each cluster we show three 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 centre (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 $I\leq 20$ 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

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6830f11a.eps}\end{figure}$ Figure 11: Colour-magnitude diagrams for the ten non-confirmed systems with V- and I-band data available. The filled circles mark galaxies inside the cluster region, while open circles mark objects in the background region. The lines mark the expected position of the red sequence at redshifts 0.1, 0.2, 0.3 and 0.4, with the solid line marking the one expected from the matched-filter estimated redshift. The second and third columns the two shifted, tilted histograms similar to the ones of Fig. 10 in the middle column. A magnitude cut of $I\leq 20$ is applied for constructing the tilted histograms.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{6830f11b.eps} \end{figure}$ Figure 11: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6830f1.eps}\end{figure}$	Figure 1: The distribution of overall completeness, the fraction of targeted galaxies to all galaxies ( upper panel), and overall efficiency, the fraction of spectra that yielded a redshift determination ( lower panel) per field. The overall completeness is defined for galaxies brighter than I=20.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6830f2.eps}\end{figure}$	Figure 2: The completeness ( upper panel) and efficiency ( lower panel) as function of magnitude as found for the clusters EISJ0049-2920 (#5, dotted line), a typical case of high efficiency, and EISJ2236-4026 (#7, dashed line), a typical case of low efficiency.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{6830f3.eps}\end{figure}$	Figure 3: Redshift distributions for the observed cluster fields as indicated in each panel. 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 (dashed line). The solid lines mark the detected groups.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6830f8.eps}\end{figure}$	Figure 8: Detailed redshift distributions for all systems considered confirmed.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6830f9.eps}\end{figure}$	Figure 9: Distribution of velocity dispersions (solid line) compared with that of the $z_{\rm MF}=0.2$ sample scaled to the same number of objects (dashed line, Paper III). The dotted histogram denote the distribution assuming that the four systems with substructure are superpositions and only the richest group is included as the confirmation.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{6830f11b.eps} \end{figure}$	Figure 11: continued.
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