All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5384fig1.ps}\end{figure}$ Figure 1: Photometric redshifts $z_{\rm phot}$ versus spectroscopic redshifts $z_{\rm spec}$ for all the galaxies in the catalogue with spectroscopic observations (Grazian et al. 2006, and refs. therein). Dashed lines indicate the rms uncertainty 0.05(1+z).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5384fig2.ps}\end{figure}$ Figure 2: a) The distribution of photometric redshifts of the sample. b) Average $\rho _{10}$ density on the entire field, in redshift bins, versus z as determined by the (2D+1) algorithm using for all sources: i) photometric redshifts (dashed line); ii) photometric redshifts, or spectroscopic redshifts whenever available (continuous line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5384fig3.ps} \end{figure}$ Figure 3: Isodensity contours of the surface density $\Sigma _{10}$ as computed in the redshift slice 0.70 < z < 0.75, which includes the first detected structure ( left panel). b) Same plot for the second structure in the redshift slice 0.90 < z <1.10 ( right panel).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5384fig4.ps} \end{figure}$ Figure 4: Galaxy colour distributions: at high density ( $\rho_{10}>0.08~{\rm Mpc}^{-3}$ ) (shaded histogram), at low density ( $\rho_{10}<0.03~{\rm Mpc}^{-3}$ ), for the two structures at $z\sim$ 0.70 ( left) and $z \sim 1.0$ ( right).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5384fig5.ps} \end{figure}$ Figure 5: Fraction of galaxies with rest frame colour B-R> 1.25 as a function of the volume density $\rho _{10}$ , for the two structures at $z\sim$ 0.70 ( left) and $z \sim 1.0$ ( right). Error bars represent Poissonian fluctuation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5384fig6.ps} \end{figure}$ Figure 6: Left panels: histograms of the C' colour, defined in the text, for all the objects in the intervals 0.7<z<0.8, 0.9<z<1.1, 1.4<z<1.7 (from the top). Dashed lines, corresponding to a local minimum, define the red and the blue populations. Right panels: rest-frame (U-V) vs. M_V diagrams: the continuous line represents the fit to the points belonging to the red population, with a fixed slope $\alpha _{\rm RS}$ = 0.08. The dashed vertical line represents the reference absolute magnitude M_V=-20.7. The dotted line indicates the valley separating the two populations.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5384fig7.ps} \end{figure}$ Figure 7: The colour $C'_{\rm RS}$ at $M_{V_{\rm rest}}$ = -20 of the average red sequence, as computed from COMBO17 survey (circles), and resulting from the present analysis (triangles). The straight line represents a linear fit on all the data analysed in the COMBO17 survey (adapted from Bell et al. 2004).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5384fig8.ps} \end{figure}$ Figure 8: The slope of the rest-frame (U-B) vs. M_B in the galaxy clusters collected by Blakeslee et al. (2003) (open squares) and in the two structures detected in the CDFS (filled squares). The dotted line represents the average value derived by Blakeslee et al. (2003).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5384fig9.ps} \end{figure}$ Figure 9: Galaxies above an environmental density $\rho _{10}$ threshold 5 times the average, for redshifts 0.5, 1.0, 1.5 and 2.0 and for catalogues with two different limiting magnitudes. Filled dots represent real members of the simulated richness class 0 clusters, while crosses represent interlopers. The contamination is reported in each panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5384fig1.ps}\end{figure}$	Figure 1: Photometric redshifts $z_{\rm phot}$ versus spectroscopic redshifts $z_{\rm spec}$ for all the galaxies in the catalogue with spectroscopic observations (Grazian et al. 2006, and refs. therein). Dashed lines indicate the rms uncertainty 0.05(1+z).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{5384fig2.ps}\end{figure}$	Figure 2: a) The distribution of photometric redshifts of the sample. b) Average $\rho _{10}$ density on the entire field, in redshift bins, versus z as determined by the (2D+1) algorithm using for all sources: i) photometric redshifts (dashed line); ii) photometric redshifts, or spectroscopic redshifts whenever available (continuous line).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{5384fig3.ps} \end{figure}$	Figure 3: Isodensity contours of the surface density $\Sigma _{10}$ as computed in the redshift slice 0.70 < z < 0.75, which includes the first detected structure ( left panel). b) Same plot for the second structure in the redshift slice 0.90 < z <1.10 ( right panel).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5384fig4.ps} \end{figure}$	Figure 4: Galaxy colour distributions: at high density ( $\rho_{10}>0.08~{\rm Mpc}^{-3}$ ) (shaded histogram), at low density ( $\rho_{10}<0.03~{\rm Mpc}^{-3}$ ), for the two structures at $z\sim$ 0.70 ( left) and $z \sim 1.0$ ( right).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5384fig5.ps} \end{figure}$	Figure 5: Fraction of galaxies with rest frame colour B-R> 1.25 as a function of the volume density $\rho _{10}$ , for the two structures at $z\sim$ 0.70 ( left) and $z \sim 1.0$ ( right). Error bars represent Poissonian fluctuation.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5384fig7.ps} \end{figure}$	Figure 7: The colour $C'_{\rm RS}$ at $M_{V_{\rm rest}}$ = -20 of the average red sequence, as computed from COMBO17 survey (circles), and resulting from the present analysis (triangles). The straight line represents a linear fit on all the data analysed in the COMBO17 survey (adapted from Bell et al. 2004).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5384fig8.ps} \end{figure}$	Figure 8: The slope of the rest-frame (U-B) vs. M_B in the galaxy clusters collected by Blakeslee et al. (2003) (open squares) and in the two structures detected in the CDFS (filled squares). The dotted line represents the average value derived by Blakeslee et al. (2003).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{5384fig9.ps} \end{figure}$	Figure 9: Galaxies above an environmental density $\rho _{10}$ threshold 5 times the average, for redshifts 0.5, 1.0, 1.5 and 2.0 and for catalogues with two different limiting magnitudes. Filled dots represent real members of the simulated richness class 0 clusters, while crosses represent interlopers. The contamination is reported in each panel.
Open with DEXTER