Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig1.ps}\end{figure}$ Figure 1: Top panel: Target Sampling Rate as a function of the x-radius for the VVDS-0226-04 field. Bottom panel: x-radius distribution in the VVDS-0226-04 photometric catalogue at $17.50 \le I_{AB} \le 24.0$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig2.ps}\end{figure}$ Figure 2: Redshift distributions normalized to unity for each spectroscopic quality flag. For high quality flags 2, 3, 4, we show both the spectroscopic redshift distributions (dashed lines) and the photometric redshift distributions (solid lines) on the same area. For quality flags 0 and 1, we show only the redshift distribution estimated using the photometric redshifts.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig3.ps}\end{figure}$ Figure 3: Spectroscopic Success Rate as a function of redshift and per apparent magnitude bin. The associated weight is shown in the bottom of each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1961fig4.ps}\end{figure}$ Figure 4: Comparison between the "unweighted'' LFs (solid triangles for 1/ $V_{\rm max}$ , solid lines for STY) and our best LF estimates ("weighted'') (open circles for 1/ $V_{\rm max}$ , dotted lines for STY) in the B rest-frame band. The best STY fits and the associated 90% error contours are shown as insets with the same symbols. We report in each inset the SDSS local estimate with open triangles.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1961fig5.ps}\end{figure}$ Figure 5: Estimate of the global LF in the U band from z = 0.05 to z = 2. The estimate is derived using the weighting scheme described in Sect. 3. We adopt the following symbols for the various estimators: circles for the 1/ $V_{\rm max}$ , triangles for the SWML, squares for the C⁺ and solid lines for the STY. The vertical short-dashed lines show the faint absolute magnitude limits considered in the STY estimate (see Sect. 4.2). In each panel, we show also the local LF derived by the SDSS (long dashed lines). The vertical dot-dashed line in the redshift bin 0.05-0.2, corresponds to the faint absolute magnitude limit surveyed by the SDSS.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1961fig6.ps}\hspace*{6mm} ... ...g8.ps}\hspace*{6mm} \includegraphics[width=7.9cm,clip]{1961fig9.ps}\end{figure}$ Figure 6: Same symbols as in Fig. 5, in the rest-frame band B ( upper-left), V ( upper-right), R ( lower-left) and I ( lower-right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1961fig10.ps}\end{figure}$ Figure 7: $M^*-\alpha$ error contours, at 90% confidence level ( $2\Delta {\rm ln}~\mathcal L=4.61$ ), obtained with the STY estimator. The solid squares are the STY best estimates. Error contours are not drawn when one of the two values has been fixed (see text). When $\alpha$ is fixed, we estimate the range of allowed M^* values, varying $\alpha$ between $\alpha =-2.0$ and $\alpha =-1.2$ . When M^* is fixed, we vary M^* by 0.5 around the set value. The error contours are shown for the U, B, V, R and I band LFs from the left to the right panels, respectively. The panels from the top to the bottom correspond to the eight redshift bins, from z=0.05 to z=2. We report with open triangles the SDSS local values (the error bars are included inside the symbols).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1961fig11.ps}\end{figure}$ Figure 8: Evolution with redshift of the ratio between the density of galaxies brighter than $M^*_{{\rm SDSS}}(z=0.1)$ and the SDSS local value.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1961fig12.ps}\end{figure}$ Figure 9: Evolution in the five bands of the parameter $\alpha$ in the top panel and of the parameter M^* in the second panel. The bottom panel shows the evolution of M^* with the slope fixed to the VVDS local value.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1961fig13.ps}\end{figure}$ Figure 10: Comparison between the CFRS and the VVDS global B-band LFs. The solid lines (STY) and the circles (1/ $V_{\rm max}$ ) correspond to the VVDS estimates. The vertical short-dashed lines are the faint absolute magnitude limits considered in the STY estimates. The long-dashed lines correspond to the CFRS estimate. The vertical dot-dashed lines correspond to the faint absolute magnitude limits surveyed by the CFRS.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1961fig14.ps}\end{figure}$ Figure 11: Comparison between the global B-band LFs derived with the HDF data (Poli et al. 2003) and with the VVDS data. The solid lines (STY) and the circles (1/ $V_{\rm max}$ ) correspond to the VVDS estimates. The vertical short-dashed lines are the faint absolute magnitude limits considered in the STY estimates. The long dashed lines correspond to the global LFs derived by Poli et al. (2003). The vertical dot-dashed lines correspond to the faint absolute magnitude limits surveyed by the HDF data.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1961fig15.ps}\end{figure}$ Figure 12: Comparison between the COMBO-17 and the VVDS global B-band LFs. The solid lines and the points correspond to the VVDS estimates. The vertical short-dashed lines are the faint absolute magnitude limits considered in the STY estimates. The long dashed lines are the global LFs derived by Wolf et al. (2003). The vertical dot-dashed lines correspond to the faint absolute magnitude limits surveyed by the COMBO-17 data. The best estimated values for the $\alpha ,M^*$ parameters measured by the VVDS are shown with solid squares in insets, and the associated 90% error contours with solid lines. The ( $\alpha ,M^*$ ) parameters given by COMBO-17 are the open stars, with error bars included inside the symbols.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig16.ps}\end{figure}$ Figure A.1: Difference between our "rederived'' absolute magnitudes and "true'' absolute magnitudes from GALICS as a function of redshift, in the U, B, V, R and I reference bands from the top to the bottom panels, respectively. The vertical lines indicate the change of Obs filter and the adopted Obs filter is labeled in the corresponding redshift range.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig1.ps}\end{figure}$	Figure 1: Top panel: Target Sampling Rate as a function of the x-radius for the VVDS-0226-04 field. Bottom panel: x-radius distribution in the VVDS-0226-04 photometric catalogue at $17.50 \le I_{AB} \le 24.0$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig2.ps}\end{figure}$	Figure 2: Redshift distributions normalized to unity for each spectroscopic quality flag. For high quality flags 2, 3, 4, we show both the spectroscopic redshift distributions (dashed lines) and the photometric redshift distributions (solid lines) on the same area. For quality flags 0 and 1, we show only the redshift distribution estimated using the photometric redshifts.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1961fig3.ps}\end{figure}$	Figure 3: Spectroscopic Success Rate as a function of redshift and per apparent magnitude bin. The associated weight is shown in the bottom of each panel.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1961fig6.ps}\hspace{6mm} ... ...g8.ps}\hspace{6mm} \includegraphics[width=7.9cm,clip]{1961fig9.ps}\end{figure}$	Figure 6: Same symbols as in Fig. 5, in the rest-frame band B ( upper-left), V ( upper-right), R ( lower-left) and I ( lower-right).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1961fig11.ps}\end{figure}$	Figure 8: Evolution with redshift of the ratio between the density of galaxies brighter than $M^*_{{\rm SDSS}}(z=0.1)$ and the SDSS local value.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1961fig12.ps}\end{figure}$	Figure 9: Evolution in the five bands of the parameter $\alpha$ in the top panel and of the parameter M^* in the second panel. The bottom panel shows the evolution of M^* with the slope fixed to the VVDS local value.
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