All Figures

$\begin{figure} \par\includegraphics[width=14.5cm,height=14cm,clip]{H4212fig1.ps} \end{figure}$ Figure 1: Completeness limits of the photometric catalogues. Total magnitudes (mag $_{\rm tot}$ ) are plotted against the magnitudes in the detection aperture (mag $_{\rm cell}$ ). The vertical and horizontal lines correspond to the detection threshold and to the completeness magnitudes respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,height=6.76cm,clip]{H4212fig2.ps} \end{figure}$ Figure 2: The cluster signal-to-noise ratio (see text and Eq. (1)) in a rich cluster at z=0.31 (filled dots and continuous line) and at z=0.64 (open squares and dotted line).
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.5cm,height=13.5cm,clip]{H4212fig3.ps} \end{figure}$ Figure 3: The completeness as a function of the magnitude of the samples used to derive the photometric redshift distribution of the galaxies in the EIS 0048 field. In each panel the vertical dotted line indicates the magnitude corresponding to $50\%$ completeness. The CLFs are computed up to the faintest magnitude bin brighter than these limits.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.5cm,height=13.5cm,clip]{H4212fig4.ps} \end{figure}$ Figure 4: The CLFs of EIS 0048 from V- to K-band (filled dots). In each panel the best-fit Schechter function is also shown (solid line).
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.5cm,height=13.5cm,clip]{H4212fig5.ps} \end{figure}$ Figure 5: Evolution of the Schechter parameter M^* in K- and V-bands as a function of redshift. In the K-band the data come from DPSE99 (empty circles), Andreon (2001, empty square), NKY01 (empty pentagon), and from this work (filled circle). In the V-band the data come from Busarello et al. (2002, empty triangle) and from this work (filled circle). In the upper panels, the dashed lines represent the NE model. The PLE models (solid lines) at different formation redshift $z_{\rm f}$ are shown in decreasing order of $z_{\rm f}$ from top to bottom. In the lower panels the PLE models (dotted lines) are shown as a function of the redshift z₉₉ at which galaxies formed the 99% of their stars (decreasing from top to bottom).
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,height=14cm,clip]{H4212fig1.ps} \end{figure}$	Figure 1: Completeness limits of the photometric catalogues. Total magnitudes (mag $_{\rm tot}$ ) are plotted against the magnitudes in the detection aperture (mag $_{\rm cell}$ ). The vertical and horizontal lines correspond to the detection threshold and to the completeness magnitudes respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,height=6.76cm,clip]{H4212fig2.ps} \end{figure}$	Figure 2: The cluster signal-to-noise ratio (see text and Eq. (1)) in a rich cluster at z=0.31 (filled dots and continuous line) and at z=0.64 (open squares and dotted line).
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$\begin{figure} \par\includegraphics[angle=0,width=13.5cm,height=13.5cm,clip]{H4212fig3.ps} \end{figure}$	Figure 3: The completeness as a function of the magnitude of the samples used to derive the photometric redshift distribution of the galaxies in the EIS 0048 field. In each panel the vertical dotted line indicates the magnitude corresponding to $50\%$ completeness. The CLFs are computed up to the faintest magnitude bin brighter than these limits.
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$\begin{figure} \par\includegraphics[angle=0,width=13.5cm,height=13.5cm,clip]{H4212fig4.ps} \end{figure}$	Figure 4: The CLFs of EIS 0048 from V- to K-band (filled dots). In each panel the best-fit Schechter function is also shown (solid line).
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