All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1215fig1.ps}\end{figure}$ Figure 1: The uppermost panel displays the positions of the 73 objects in the cluster line-of-sight that were originally selected for spectroscopy (see text). Symbol size is proportional to each galaxy's flux in the I-band (as computed from the aperture magnitude referred to in Sect. 2.1). The middle panel shows the positions of the 54 galaxies for which spectra was obtained and a reliable redshift was measured - listed in Table 2. Symbol size is, again, proportional to each galaxy's flux in the I-band (and is listed in Col. 10 of Table 2). Galaxies with no magnitude measure available (i.e. with identification number larger than 900) are noted by an open symbol (size, in these cases, is arbitrary). The lower panel maps the positions of the 23 galaxies belonging to the cluster (see Sect. 4). The cluster centre, as defined by the cluster detection algorithm, is identified by the cross.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{1215fig2.ps}\end{figure}$ Figure 2: Histogram of redshifts for all 54 galaxies in the cluster field with a line-of-sight velocity measure.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1215fig6.ps}\end{figure}$ Figure 6: Positions of the 19 cluster member galaxies for which the population synthesis method converged. Each symbol denotes belonging to one of the 3 different cluster regions, set according to projected distance to the centre (marked by a cross): from diamonds, through triangles up to squares we are moving outwards from the core, through the intermediate regions and to the outskirts (as far out as the cluster virial radius) of projected cluster regions.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1215fig7.ps}\end{figure}$ Figure 7: Gradient trends found within the cluster (ranging from the centre through the intermediate region and far out till the outskirts) in terms of the three main population components: old main sequence, intermediate giants and supergiant stars (indicated in percentages). Asterisks denote the mean of the values of each region.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1215fig8.ps}\end{figure}$ Figure 8: Comparison between the population found: in the field galaxies ( upper left); in the cluster as a whole ( upper right); in the cluster centre ( bottom left) and in the cluster outskirts ( bottom right). The standard deviations of the values of these averages vary between 13% and 23%.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1215fig9.ps}\end{figure}$ Figure 9: R-I colour as a function of cluster-centric projected distance for all cluster galaxies having reliable photometry. For these objects the mean value of the error in the R-I colour is $\sim$ 0.03 mag. Open symbols are the same as in Fig. 6, indicating the cluster-centric distance class in which a galaxy is considered. Filled symbols give, at mean distance for each class, the mean colour of that class (the "error bar'' indicates the dispersion of the values used to compute the average). Smaller dots refer to field galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1215fi10.ps}\end{figure}$ Figure 10: Colours versus distance to the centre of the cluster. The symbols sizes are proportional to the percentages of the 3 stellar population components indicated in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1215fig3.ps}\end{figure}$ Figure 3: Stellar population found for the 44 objects, 19 in the cluster ( left panels) and 25 in the field ( right panels). In abcissae we have plotted the 6 population components defined (see text): yd - young dwarfs; id - intermediate dwarfs; od - old dwarfs; yg - young giants; ig - intermediate giants and sg - supergiants.
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In the text

$\begin{figure}\par\includegraphics[width=8cm,clip]{1215f4_1.ps}\hspace*{4mm} \includegraphics[width=8cm,clip]{1215f4_2.ps}\end{figure}$ Figure 4: Spectra of the cluster galaxies (black line) in the rest-frame superimposed to the respective synthetic spectra (red line) computed with the results of the GPG algorithm. All fluxes are relative values.
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In the text

$\begin{figure}\par\includegraphics[width=7.5cm,clip]{1215f5_1.ps}\hspace*{4mm} \... ...ce*{6cm}\includegraphics[width=4cm,clip]{1215f5_3.ps}\hspace*{6cm}} \end{figure}$ Figure 5: Spectra of the field galaxies (black line) in the rest-frame superimposed to the synthetic ones (red line) computed with the results of the GPG algorithm. All fluxes are relative values.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{1215fig2.ps}\end{figure}$	Figure 2: Histogram of redshifts for all 54 galaxies in the cluster field with a line-of-sight velocity measure.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1215fig7.ps}\end{figure}$	Figure 7: Gradient trends found within the cluster (ranging from the centre through the intermediate region and far out till the outskirts) in terms of the three main population components: old main sequence, intermediate giants and supergiant stars (indicated in percentages). Asterisks denote the mean of the values of each region.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1215fig8.ps}\end{figure}$	Figure 8: Comparison between the population found: in the field galaxies ( upper left); in the cluster as a whole ( upper right); in the cluster centre ( bottom left) and in the cluster outskirts ( bottom right). The standard deviations of the values of these averages vary between 13% and 23%.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1215fi10.ps}\end{figure}$	Figure 10: Colours versus distance to the centre of the cluster. The symbols sizes are proportional to the percentages of the 3 stellar population components indicated in each panel.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{1215fig3.ps}\end{figure}$	Figure 3: Stellar population found for the 44 objects, 19 in the cluster ( left panels) and 25 in the field ( right panels). In abcissae we have plotted the 6 population components defined (see text): yd - young dwarfs; id - intermediate dwarfs; od - old dwarfs; yg - young giants; ig - intermediate giants and sg - supergiants.
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$\begin{figure}\par\includegraphics[width=8cm,clip]{1215f4_1.ps}\hspace*{4mm} \includegraphics[width=8cm,clip]{1215f4_2.ps}\end{figure}$	Figure 4: Spectra of the cluster galaxies (black line) in the rest-frame superimposed to the respective synthetic spectra (red line) computed with the results of the GPG algorithm. All fluxes are relative values.
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$\begin{figure}\par\includegraphics[width=7.5cm,clip]{1215f5_1.ps}\hspace{4mm} \... ...ce{6cm}\includegraphics[width=4cm,clip]{1215f5_3.ps}\hspace*{6cm}} \end{figure}$	Figure 5: Spectra of the field galaxies (black line) in the rest-frame superimposed to the synthetic ones (red line) computed with the results of the GPG algorithm. All fluxes are relative values.
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