All Figures

$\begin{figure} \par\includegraphics[width=9cm]{8182fi01.ps} \end{figure}$ Figure 1: Comparison of the stellar mass vs. rest-frame B band relation in 3 redshift ranges between mock catalogues (black points) and VVDS data (red points).
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{8182fi02.ps} \end{figure}$ Figure 2: Construction of the completeness limit from VVDS data in the narrow redshift range z=[0.8-0.9]. The central panel shows the value of B-band luminosity vs. the computed stellar mass for all galaxies in that redshift range. The long-dashed horizontal line defines the minimum galaxy luminosity above which stand 95% of the galaxies. The top horizontal dashed line defines the upper limit in which we compute the mean and standard deviation of the stellar mass distribution of galaxies ( top panel) standing in a luminosity interval of $\Delta M_B=0.35$ . The right-hand dashed vertical line defines the 84% completeness limit in stellar mass.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{8182fi03.ps} \end{figure}$ Figure 3: Distribution of stellar masses as a function of redshift, in the range [0.5-1.2]. The top (bold) solid line, computed from the observed scatter in the luminosity-mass relation, defines the limit above which samples are better than 84% complete. The bottom line defines the 50% completeness limit. The two dashed lines represent the same limits but derived from the Millennium simulation.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{8182fi04.ps} \end{figure}$ Figure 4: Mean luminosity and color distributions, with their $1\sigma$ variance, for galaxies with stellar masses in the range $\log~(M/M_\odot)=[9$ -9.5] in the full millennium mock catalogues, for 3 consecutive redshift ranges between z=0.5 and z=1.2. Solid red distributions correspond to galaxies fainter than I_AB=24, while hatched blue distributions correspond to galaxies brighter than this threshold. The distribution have been normalized to the total number of galaxies in each redshift range. The galaxies missed due to the I_AB=24 flux limit function are clearly intrinsically fainter and relatively redder.
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{8182fi05.ps} \end{figure}$ Figure 5: Effect of mass incompleteness on the projected correlation function $w_{\rm p}(r_{\rm p})$ estimated using the Millennium mock catalogues for the 8 mass ranges. The points give at each scale $r_{\rm p}$ the mean ratio of the correlation functions $w_{\rm p}(r_{\rm p})$ measured for a sample complete in stellar mass and its corresponding sub-sample selected in apparent magnitude $17.5\le I_{AB}\le 24$ . Error bars correspond to the rms scatter among the mocks.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi06.ps} \end{figure}$ Figure 6: ( Left) Measurements of the projected correlation function $w_{\rm p}(r_{\rm p})$ of galaxies with different stellar masses: $\log~(M/M_\odot)\ge 9.0$ ( open blue squares), $\ge$ 9.5 ( filled red squares), $\ge$ 10.0 ( open green triangles) and $\ge$ 10.5 ( filled magenta triangles) from VVDS data in the redshift range [0.5-1.2]. (Right) The best-fit parameters (r₀ and $\gamma$ ) with their associated 1-, 2- and $3\sigma$ error contours, derived from the variance among 40 mock catalogues. In this plot, no correction for the effect of incompleteness in mass is applied (see text). Note however that the correction would affect both r₀ and $\gamma$ and, for example, move the open square (the most affected one) in the right panel without modifying the observed trend.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{8182fi07.ps} \par\end{figure}$ Figure 7: Correlation length and slope measured from VVDS data at ${z\sim 0.85}$ as a function of the median stellar mass of each samples. Left and right panels refer respectively to the differential and integrated samples. Filed symbols indicate measurement non-corrected by stellar mass incompleteness, while open symbols are.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi08.ps} \end{figure}$ Figure 8: Comparison of the projected correlation function $w_{\rm p}(r_{\rm p})$ from SDSS data at $z\sim 0.15$ ( black cross; Li et al. 2006) to VVDS measurement at ${z\sim 0.85}$ ( magenta filled dots and solid lines) in 3 differential ranges of stellar masses. The green dashed line is a power-law reference line drawn with r₀=5 h^-1 Mpc and $\gamma =1.8$ . Error bars on VVDS measurement have been estimated from the variance among 40 mock catalogues. Blue open circles indicate VVDS measurements corrected for stellar mass incompleteness.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi09.ps} \end{figure}$ Figure 9: Comparison of the VVDS measurements of the projected correlation function $w_{\rm p}(r_{\rm p})$ as a function of stellar mass (filled circles), with that obtained from 40 mock VVDS surveys constructed from the Millennium Simulation. The dashed area describes the rms among the 40 simulated catalogues.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi10.ps} \end{figure}$ Figure 10: The redshift evolution of the linear bias for galaxies of different stellar mass, obtained from the SDSS ( $z\sim 0.15$ , open squares, Li et al. 2006), and the VVDS ( ${z\sim 0.85}$ , filled squares, this work).
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{8182fi01.ps} \end{figure}$	Figure 1: Comparison of the stellar mass vs. rest-frame B band relation in 3 redshift ranges between mock catalogues (black points) and VVDS data (red points).
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$\begin{figure} \par\includegraphics[width=9cm]{8182fi07.ps} \par\end{figure}$	Figure 7: Correlation length and slope measured from VVDS data at ${z\sim 0.85}$ as a function of the median stellar mass of each samples. Left and right panels refer respectively to the differential and integrated samples. Filed symbols indicate measurement non-corrected by stellar mass incompleteness, while open symbols are.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi09.ps} \end{figure}$	Figure 9: Comparison of the VVDS measurements of the projected correlation function $w_{\rm p}(r_{\rm p})$ as a function of stellar mass (filled circles), with that obtained from 40 mock VVDS surveys constructed from the Millennium Simulation. The dashed area describes the rms among the 40 simulated catalogues.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{8182fi10.ps} \end{figure}$	Figure 10: The redshift evolution of the linear bias for galaxies of different stellar mass, obtained from the SDSS ( $z\sim 0.15$ , open squares, Li et al. 2006), and the VVDS ( ${z\sim 0.85}$ , filled squares, this work).
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