All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3449fig1.eps} \end{figure}$ Figure 1: VGCF and PDCS clusters. We draw with a thick line our clusters, with a dashed line PDCS clusters, with a thin line the VGCF detections in individual bands (the radii of these last detections are arbitrary. VGCF clusters are labeled with their ID number, PDCS clusters are labeled with A "P'' followed by the PDCS identification number.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{3449fig4.eps} \end{figure}$ Figure 4: R band images of cluster V05 ( left panel) and cluster V10 ( right panel). ETS reveal clusters at z = 0.7 and z = 0.6, respectively. The central galaxies in these images correspond to brighter galaxies in the ETS of these systems. North is up and East is left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{3449fig5.eps} \end{figure}$ Figure 5: (B-R, R) CMD of clusters P33, P36 and P63. The ETS are linear fits with constant slopes to black filled circles and crosses. Crosses are cluster members with spectroscopic redshift.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3449fig6.eps} \end{figure}$ Figure 6: Comparison between VGCF and PDCS redshift estimates. The diagonal line illustrates a one-to-one relation and it is not a fit.
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{3449fig2.eps} \end{figure}$ Figure 2: (B-R, R) and (V-I, I) ETS and redshift estimates of clusters within our survey. This sample includes clusters with ETS in both (B-R, R) and (V-I, I) diagrams.
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{3449fig3.eps} \end{figure}$ Figure 3: ETS and redshift estimates of clusters within our survey. This sample includes clusters with ETS in only one of either (B-R, R) or (V-I, I) diagrams.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3449fig1.eps} \end{figure}$	Figure 1: VGCF and PDCS clusters. We draw with a thick line our clusters, with a dashed line PDCS clusters, with a thin line the VGCF detections in individual bands (the radii of these last detections are arbitrary. VGCF clusters are labeled with their ID number, PDCS clusters are labeled with A "P'' followed by the PDCS identification number.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{3449fig4.eps} \end{figure}$	Figure 4: R band images of cluster V05 ( left panel) and cluster V10 ( right panel). ETS reveal clusters at z = 0.7 and z = 0.6, respectively. The central galaxies in these images correspond to brighter galaxies in the ETS of these systems. North is up and East is left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16cm,clip]{3449fig5.eps} \end{figure}$	Figure 5: (B-R, R) CMD of clusters P33, P36 and P63. The ETS are linear fits with constant slopes to black filled circles and crosses. Crosses are cluster members with spectroscopic redshift.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{3449fig6.eps} \end{figure}$	Figure 6: Comparison between VGCF and PDCS redshift estimates. The diagonal line illustrates a one-to-one relation and it is not a fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{3449fig2.eps} \end{figure}$	Figure 2: (B-R, R) and (V-I, I) ETS and redshift estimates of clusters within our survey. This sample includes clusters with ETS in both (B-R, R) and (V-I, I) diagrams.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{3449fig3.eps} \end{figure}$	Figure 3: ETS and redshift estimates of clusters within our survey. This sample includes clusters with ETS in only one of either (B-R, R) or (V-I, I) diagrams.
Open with DEXTER