All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[width=9cm]{7959fig1.ps}} \end{figure}$ Figure 1: Left panel: colour-magnitude diagrams in various redshift intervals; the lines represent the best-fit relations for the blue and red populations and the locus of the minimum, the shaded area is the uncertainty on the minimum. Right panel: the histograms of colour distribution projected at M_B=-20 along the best-fit correlations, the continuous horizontal lines are the colour separation at this magnitude, and the dash horizontal lines are the loci of the maxima.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig2.ps}} \end{figure}$ Figure 2: As in Fig. 1 but for the SSFR-magnitude distribution.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig3.ps}} \end{figure}$ Figure 3: Volume corrected colour histogram, in four bins of magnitude, in the redshift interval 0.4<z<0.7. The continuous lines are the double-Gaussian fit to the colour distributions.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig4.ps}} \end{figure}$ Figure 4: Points are the minima obtain by the fits shown in Fig. 3. Continuous line is the linear fit to these minima.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig5.ps}} \end{figure}$ Figure 5: Total LF as a function of redshift. The continuous curves come from our maximum likelihood analysis. The dotted line is the local LF (Norberg et al. 2002). The filled circles are the points obtained with 1/V_MAX method. The empty circles come from the DEEP2 survey (Willmer et al. 2006). The results from the COMBO17 and VDDS surveys are consistent with the DEEP2 results and are omitted from the plot. The dashed-point line is the model of Menci et al. (2006).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig6.ps}} \end{figure}$ Figure 6: LFs of the blue galaxies as function of redshift. The continuous curves comes from our maximum likelihood analysis. The dotted line is our fit at $z\sim 0.3$ , reported for comparison in all the redshift bins. The big filled circles are the points obtained with 1/V_MAX method. The small empty circles are points from the LFs by Willmer et al. (2006).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig7.ps}} \end{figure}$ Figure 7: LFs of the red galaxies as function of redshift. The continuous curves comes from our maximum likelihood analysis. The first bin of redshift, has been excluded from this evolutive analysis since the statistics are too low. The dotted line is our fit at $z\sim 0.5$ , reported for comparison in all the redshift bins. The big filled circles are the points obtained with 1/V_MAX method. The small empty circles are points from the LFs by Willmer et al. (2006). The dashed-point orange line is the model of Menci et al. (2006).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig8.ps}} \end{figure}$ Figure 8: LFs of the red galaxies. The filled circles indicate the LF obtained with the linear colour selection in Table 2. The empty circles indicate the LF obtained from the colour histograms in bins of magnitude (see Figs. 3 and 4).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig9.ps}} \end{figure}$ Figure 9: LFs of the early type galaxies as a function of redshift. The continuous curves comes from our maximum likelihood analysis. The dotted line is our fit at $z\sim 0.5$ , reported for comparison in all the redshift bins. The big filled circles are the points obtained with $1/V_{\rm MAX}$ method.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig10.ps}} \end{figure}$ Figure 10: Upper panel: galaxy luminosity density for red (filled squares) and blue galaxies (empty squares). Lower panel: the same as the upper panel but for early type galaxies (filled squares) and late type galaxies (empty squares). Small points are the local luminosity density estimates by Madgwick et al. (2002) (z=0.04) and Bell et al. (2003) (z=0.07).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig11.ps}} \end{figure}$ Figure 11: Panel a): stellar mass distribution for the early and late population, the area of each histogram is normalised to unity. The arrows indicate the mean value of the stellar mass for the early population (thin arrow) and for the late population (thick arrow). Panel b): as for panel a) but for the distribution of $\rho /\rho _{\rm med}$ . Panel c): early type galaxies vs. late type galaxies fraction as a function of the density contrast ( $\rho /\rho _{\rm ed}$ ).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig2.ps}} \end{figure}$	Figure 2: As in Fig. 1 but for the SSFR-magnitude distribution.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig3.ps}} \end{figure}$	Figure 3: Volume corrected colour histogram, in four bins of magnitude, in the redshift interval 0.4<z<0.7. The continuous lines are the double-Gaussian fit to the colour distributions.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig4.ps}} \end{figure}$	Figure 4: Points are the minima obtain by the fits shown in Fig. 3. Continuous line is the linear fit to these minima.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig6.ps}} \end{figure}$	Figure 6: LFs of the blue galaxies as function of redshift. The continuous curves comes from our maximum likelihood analysis. The dotted line is our fit at $z\sim 0.3$ , reported for comparison in all the redshift bins. The big filled circles are the points obtained with 1/V_MAX method. The small empty circles are points from the LFs by Willmer et al. (2006).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig8.ps}} \end{figure}$	Figure 8: LFs of the red galaxies. The filled circles indicate the LF obtained with the linear colour selection in Table 2. The empty circles indicate the LF obtained from the colour histograms in bins of magnitude (see Figs. 3 and 4).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig9.ps}} \end{figure}$	Figure 9: LFs of the early type galaxies as a function of redshift. The continuous curves comes from our maximum likelihood analysis. The dotted line is our fit at $z\sim 0.5$ , reported for comparison in all the redshift bins. The big filled circles are the points obtained with $1/V_{\rm MAX}$ method.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7959fig10.ps}} \end{figure}$	Figure 10: Upper panel: galaxy luminosity density for red (filled squares) and blue galaxies (empty squares). Lower panel: the same as the upper panel but for early type galaxies (filled squares) and late type galaxies (empty squares). Small points are the local luminosity density estimates by Madgwick et al. (2002) (z=0.04) and Bell et al. (2003) (z=0.07).
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