All Figures

$\begin{figure} \par\includegraphics[bb=25 170 390 420,width=8.8cm,clip]{8735F01.eps} \end{figure}$ Figure 1: The combined selection function for the whole sample. The histograms show the I-band magnitude distribution for the photometric (dashed red line) and spectroscopic (blue solid line). The points show the fraction of galaxies for which we derived redshifts. The error bars are Poisson distributed errors (Gehrels 1986).
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In the text

$\begin{figure} \par\includegraphics[bb=25 160 350 400,width=8.6cm,clip]{8735F02.eps} \end{figure}$ Figure 2: V-band apparent magnitude versus continuum signal-to-noise ratio as measured in Sect. 2.5. Open red diamonds are galaxies without emission lines, whereas filled blue diamonds are galaxies with at least one emission line.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8735F03.eps} \end{figure}$ Figure 3: Redshift distribution of the targets in the three fields, with the cluster names marked. The small arrows mark the position of the group candidates (see Sect. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8735F04.eps} \end{figure}$ Figure 4: Color-magnitude diagrams of the members of the six observed clusters. Filled blue diamonds are star-forming galaxies, whereas open red diamonds are passive galaxies. The shaded areas are defined by the 3- $\sigma$ deviation of the least squares fits to the passive galaxies. The vertical dashed line mark $M_I\approx -21.4$ used in the density calculation (see Sect. 3.5). We note the red star-forming galaxies belonging to the red-sequence and even redder in some of the clusters.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,bb=20 160 360 400,clip]{8735F05.eps} \end{figure}$ Figure 5: Bolometric X-ray luminosity plotted against velocity dispersion. Open circles (Markevitch 1998), crosses (David et al. 1993) and stars (Xue & Wu 2000) represent the $L_{\rm X}-\sigma$ relation for local clusters. The six clusters studied here are plotted as diamonds with error bars in the velocity dispersion.
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In the text

$\begin{figure} \par\includegraphics[bb=20 155 600 430,width=8.8cm,clip]{8735F06.eps} \end{figure}$ Figure 6: Relation between virial radius and projected density before and after correction for field contamination. The open red circles are passive galaxies, whereas filled blue circles are star-forming galaxies.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7cm]{8735F07a.eps}\includegraphi... ...dth=7cm]{8735F07c.eps}\includegraphics[width=7cm]{8735F07d.eps} }\end{figure}$ Figure 7: Representation of the fields of the observed clusters as indicated by the names on the individual figures. Only cluster members are shown. Blue filled and open red symbols represent star-forming and passive galaxies respectively. The cluster centers are marked with large vertical crosses and the large concentric circles represent one and two virial radii respectively. The contours are the density maps of all galaxies with colors compatible with the red-sequence of the respective cluster (see Sect. 4). The arrows in the VMF194 plot indicate the position of a rich background group (see Sect. 4.1).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7cm]{8735F07e.eps}\includegraphics[width=7cm]{8735F07f.eps} }\end{figure}$ Figure 7: continued. Representation of the observed clusters as indicated by the names on the individual figures. Only cluster members are shown. Blue filled symbols are star-forming galaxies and open red are passive ones. The arrows in VMF73 show the position of the X-ray structure detected by Rasmussen & Ponman (2004) (see Sect. 4.3).
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In the text

$\begin{figure} \par\includegraphics[bb=30 165 325 420,width=4cm,clip]{8735F08a.eps} \includegraphics[bb=30 165 325 420,width=4cm,clip]{8735F08b.eps} \end{figure}$ Figure 8: Fraction of blue cluster galaxies (as defined in Sect. 5.1) against normalized virial radius and projected density.
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In the text

$\begin{figure} \par\includegraphics[bb=20 155 325 420,width=5cm,clip]{8735F09a.e... ... \includegraphics[bb=20 155 325 420,width=5cm,clip]{8735F09f.eps} \end{figure}$ Figure 9: Fraction of star-forming galaxies (left panels) and mean EWs of [O II] ( middle panels) and H $\alpha$ ( right panels) against normalized clustercentric distances ( top panels) and projected densities to the 5 ${\rm th}$ neighbor ( $\ensuremath {\Sigma _5}$ , bottom panels), plotted as the thick, solid, black lines. The shaded areas around the curve in light blue are the standard deviations of the bootstrapped values. The horizontal areas show the field values for galaxies between 0.15<z<0.35.
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In the text

$\begin{figure} \par\includegraphics[bb=25 155 325 420,width=5cm,clip]{8735F10a.e... ... \includegraphics[bb=25 155 325 420,width=5cm,clip]{8735F10d.eps} \end{figure}$ Figure 10: Similar to Fig. 9 but now analyzing the distribution of the star-forming population only (i.e. $\ensuremath{W_0(\mbox{[O{\sc ii}]},\mbox{H$\alpha$ })} >5$ Å).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{8735F11a.eps} \includegraphics[width=8cm]{8735F11b.eps} } \end{figure}$ Figure 11: Fraction of star-forming galaxies and mean equivalents widths against normalized cluster distance and projected density for the clusters VMF73 and VMF131 as depicted in the respective panels. In the bottom panels, dashed blue lines are for $\ensuremath{\langle \ensuremath{W_0(\mbox{[O{\sc ii}]})} \rangle}$ and solid red lines for $\ensuremath{\langle \ensuremath{W_0(\mbox{H$\alpha$ })} \rangle}$ bottom panels the dashed blue line represent the mean [O II] EWs and the solid red line the H $\alpha$ ones. The respective 1- $\sigma$ are marked as the hashed areas in the bottom panels and thin dotted lines in top panels.
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In the text

$\begin{figure} \par\includegraphics[bb=20 150 470 470,width=8.8cm,clip]{8735F12.eps} \end{figure}$ Figure 12: Line ratio diagnostic diagrams to identify AGNs. The left panel is the BPT plane showing the relation between four emission lines. The dashed and dotted curves separate AGNs from star-forming galaxies (see text). The vertical and horizontal lines are the approximate separation between types. The lower right panel is the [O II]-H $\alpha$ diagram aimed to identify LINERs. The dotted line is the local Kennicutt's relation for star-forming galaxies, whereas the dashed line is the test to identify LINERs. The upper right panel is the relation between [N II] and H $\alpha$ EWs. Blue open circles are ``normal'' star-forming galaxies and red filled ones are the red star-forming galaxies. The size of the symbols is related to the confidence with which each index can be measured, the larger the better.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8735F13.eps} \end{figure}$ Figure 13: Specific star formation rates for field ( top) and cluster ( bottom) galaxies, versus stellar mass. Normal star-forming galaxies are plotted with blue filled stars and the red star-forming galaxies with green pentagons. The red open stars are passive galaxies with $0<\ensuremath{W_0(\mbox{[O{\sc ii}]},\mbox{H$\alpha$ })} <5$ and are shown for comparison. The black circles are the AGN candidates. The thick line is the local relation from Salim et al. (2007).
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8735FA1.eps} \end{figure}$ Figure A.1: Specific star formation rates based on [O II] and H $\alpha$ respectively calculated using the relations indicated in the text. Blue filled triangles are galaxies with $\ensuremath{W_0(\mbox{[O{\sc ii}]},\mbox{H$\alpha$ })} >5$ Å, classified here as star forming. The thick line is the fit to the H $\alpha$ relation: $\log(sS\!FR)\approx1.07\log(\ensuremath{W_0(\mbox{H$\alpha$ })} -11.4$ , which is plotted in the [O II] panel for comparison. Note that the $sS\!FR$ obtained with the [O II] line may be slightly overestimated.
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In the text

$\begin{figure} \par\includegraphics[bb=25 170 390 420,width=8.8cm,clip]{8735F01.eps} \end{figure}$	Figure 1: The combined selection function for the whole sample. The histograms show the I-band magnitude distribution for the photometric (dashed red line) and spectroscopic (blue solid line). The points show the fraction of galaxies for which we derived redshifts. The error bars are Poisson distributed errors (Gehrels 1986).
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$\begin{figure} \par\includegraphics[bb=25 160 350 400,width=8.6cm,clip]{8735F02.eps} \end{figure}$	Figure 2: V-band apparent magnitude versus continuum signal-to-noise ratio as measured in Sect. 2.5. Open red diamonds are galaxies without emission lines, whereas filled blue diamonds are galaxies with at least one emission line.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8735F03.eps} \end{figure}$	Figure 3: Redshift distribution of the targets in the three fields, with the cluster names marked. The small arrows mark the position of the group candidates (see Sect. 4).
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$\begin{figure} \par\includegraphics[width=8.8cm,bb=20 160 360 400,clip]{8735F05.eps} \end{figure}$	Figure 5: Bolometric X-ray luminosity plotted against velocity dispersion. Open circles (Markevitch 1998), crosses (David et al. 1993) and stars (Xue & Wu 2000) represent the $L_{\rm X}-\sigma$ relation for local clusters. The six clusters studied here are plotted as diamonds with error bars in the velocity dispersion.
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$\begin{figure} \par\includegraphics[bb=20 155 600 430,width=8.8cm,clip]{8735F06.eps} \end{figure}$	Figure 6: Relation between virial radius and projected density before and after correction for field contamination. The open red circles are passive galaxies, whereas filled blue circles are star-forming galaxies.
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$\begin{figure} \par\mbox{\includegraphics[width=7cm]{8735F07e.eps}\includegraphics[width=7cm]{8735F07f.eps} }\end{figure}$	Figure 7: continued. Representation of the observed clusters as indicated by the names on the individual figures. Only cluster members are shown. Blue filled symbols are star-forming galaxies and open red are passive ones. The arrows in VMF73 show the position of the X-ray structure detected by Rasmussen & Ponman (2004) (see Sect. 4.3).
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$\begin{figure} \par\includegraphics[bb=30 165 325 420,width=4cm,clip]{8735F08a.eps} \includegraphics[bb=30 165 325 420,width=4cm,clip]{8735F08b.eps} \end{figure}$	Figure 8: Fraction of blue cluster galaxies (as defined in Sect. 5.1) against normalized virial radius and projected density.
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$\begin{figure} \par\includegraphics[bb=25 155 325 420,width=5cm,clip]{8735F10a.e... ... \includegraphics[bb=25 155 325 420,width=5cm,clip]{8735F10d.eps} \end{figure}$	Figure 10: Similar to Fig. 9 but now analyzing the distribution of the star-forming population only (i.e. $\ensuremath{W_0(\mbox{[O{\sc ii}]},\mbox{H$\alpha$ })} >5$ Å).
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