Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig1.ps} \end{figure}$ Figure 1: The planned layout and identification numbers of the VIMOS pointings for the VVDS "Deep'' survey in the VVDS-02h. A total of 66 pointings is planned, placed on a grid with (2, 2) arcmin spacing in ( $\alpha$ , $\delta$ ). This layout allows observation of the central area (cross hatched) 4 times, and edge areas twice (hatched) except for the 4 corners which are observed once (triple hatched). See Table 2 for the list of already observed fields and Fig. 12 for the layout of objects already observed.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1960fig2.ps} \end{figure}$ Figure 2: Distribution of slit length in 6 of the VVDS-02h pointings.
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In the text

$\begin{figure} \par\includegraphics[width=15.3cm,clip]{1960fig3.ps} \end{figure}$ Figure 3: Typical layout of spectra in the 4 quadrants of a VVDS-Wide pointing; more than 550 are observed on average.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig4.ps} \end{figure}$ Figure 4: Difference between the photometric I band magnitude and the I-band magnitude computed from $\sim$ 1000 calibrated VVDS spectra. The difference is mainly due to slit losses; no systematic effect in the spectrophotometric calibration is observed vs. magnitude.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig5.ps} \end{figure}$ Figure 5: Flux-calibrated VVDS spectra compared to the photometry of the VVDS imaging survey after scaling to match to the I band flux (black dots). The spectrophotometric accuracy is conserved over the full wavelength coverage at the 10% level.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig6.ps} \end{figure}$ Figure 6: S/N per spectral resolution element over the magnitude range of the VVDS-Deep survey.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1960fig7.ps} \end{figure}$ Figure 7: Spectrum of an absorption line galaxy with I_AB=23.61, and z=3.2950, demonstrating the ability of low spectral resolution $R\sim 230$ to measure redshifts from absorption line galaxies down to the very faint end of the survey.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1960fig8.ps} \end{figure}$ Figure 8: Redshift distribution of flag 2 objects (dashed), compared to the normalized redshift distribution of the flag 3 and 4 objects (open).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig9.ps} \end{figure}$ Figure 9: Redshift distribution of flag 1 objects (dashed), compared to the normalized redshift distribution of the flag 2, 3 and 4 objects (open).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig10.ps} \end{figure}$ Figure 10: Comparison of spectroscopic redshifts vs. photometric redshifts computed from BVRI photometry for objects with magnitude $17.5 \leq I_{AB} \leq 22.5$ , for each of the quality flags 1, 2, 3 and 4 ( from bottom left to top right). The fraction of galaxies for which the difference in photometric redshift vs. spectroscopic redshift is less than 0.2 is indicated on the top of each panel. Flags 3 and 4 represent very secure redshift measurements as indicated by the comparison of objects observed spectroscopically twice (see text), hence the dispersion observed for these flags is representative of the error in measuring photometric redshifts. For flags 2 and 1, errors from the photometric redshift estimate and the spectroscopic measurements combine to provide a lower value of 16% and 42% of discrepant redshifts, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig11.ps} \end{figure}$ Figure 11: Same as Fig. 10 for objects with magnitude $22 \leq I_{AB} \leq 24$ , for each of the quality flags 1, 2, 3 and 4 ( from bottom left to top right), in the VVDS-02h area where K band data is available in addition to BVRI data and makes the photometric redshifts more accurate. The fraction of concordant redshifts is 38%, 72%, 82% and 91% for flags 1, 2, 3 and 4 respectively. Taking into account a photometric redshift failure of $\sim$ 9% as shown by the fraction of concordant flag 4 which are known to be $\sim$ 100% accurate from spectroscopy, we find that flags 1, 2 and 3 are 47%, 81%, 91% correct, respectively, in this faint magnitude regime where the accuracy of photometric redshifts rapidly decreases.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig12.ps} \end{figure}$ Figure 12: Distribution of galaxies observed in VVDS-02h.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig13.ps} \end{figure}$ Figure 13: Number and fraction of objects observed in the VVDS-02h, compared to the total number of objects in the photometric catalog with $17.5 \leq I_{AB} \leq 24$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig14.ps} \end{figure}$ Figure 14: Difference in redshift measurements for 266 galaxies observed twice in the VVDS-02h and 139 galaxies observed twice in the VVDS-CDFS. The difference has a Gaussian distribution with $\sigma _z=13 \times 10^{-4}$ or 390 km s^-1, hence each single redshift measurement has an accuracy 390/(2)^0.5 or 276 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig15.ps} \end{figure}$ Figure 15: Difference in redshift measurements for 33 objects in common between the VVDS-CDFS sample and the FORS2-GOODS observations of Vanzela et al. (2004). The difference has a mean d $z=8.4\times 10^{-4}$ and a $\sigma _z=12.6 \times 10^{-4}$ or 378 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1960fig16.ps} \end{figure}$ Figure 16: Completeness of the $I_{AB} \leq 24$ sample in the VVDS-02h field. ( Bottom panel) the magnitude distribution of galaxies with flags 0, 1, 2, 3+4 and 9; ( central panel) the magnitude distribution of galaxies with all flags (open histogram), compared to the distribution of flags 1 and 2 (filled); ( top panel) the ratio of secure redshift measurements with flags 2, 3, 4, 9 and of all measurements (filled). The overall redshift measurement completeness is 78% (flags 2, 3, 4, 9) and redshifts are measured for 93% of the sample (including flags 1).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig17.ps} \end{figure}$ Figure 17: VVDS spectra in the range $0 < z \leq 0.7$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig18.ps} \end{figure}$ Figure 18: VVDS spectra in the range $0.7 < z \leq 1.3$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig19.ps} \end{figure}$ Figure 19: VVDS spectra in the range $1.3 < z \leq 2.2$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig20.ps} \end{figure}$ Figure 20: VVDS spectra in the range $2.2 < z \leq 5$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig21.ps} \end{figure}$ Figure 21: Absolute M_{B_AB} magnitude vs. redshift in VVDS-02h. The full sample is shown together with the tracks of CWW templates (Coleman et al. 1980) and starburst templates used to compute the k(z) correction. At high redshift, the bluest tracks (starburst galaxies) correspond to the faintest absolute M_B magnitudes. Each track has been normalized to produce I_AB=24at all redshifts. As redshift increases, the computation of k(z) for the rest frame B band becomes increasingly difficult to constrain, hence produces a large range in B-band absolute luminosities for $z\geq 2$ . At these high redshifts, and given the wavelength coverage of our spectroscopy and photometry, it is more appropriate to compute absolute magnitudes in the near UV.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig22.ps} \end{figure}$ Figure 22: Redshift distribution for a magnitude-limited sample of 3621 galaxies with $17.5 \leq I_{AB} \leq 22.5$ , extracted from the sum of the VVDS-CDFS and the VVDS-F02h fields. Galaxies with flags 2, 3, 4 and 9 are represented by the filled histogram, galaxies with flag 1 by the open histogram. This sample, including flags 2, 3, 4 and 9, is 93% complete. The median redshift is z=0.62 and the mean redshift is z=0.65.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig23.ps} \end{figure}$ Figure 23: Same as Fig. 22 for 5124 galaxies with $17.5 \leq I_{AB}\leq 23$ . This sample, including flags 2, 3, 4 and 9, is 90% complete. The median redshift is z=0.67 and the mean redshift is z=0.72.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig24.ps} \end{figure}$ Figure 24: Same as Fig. 22 for 7054 galaxies with ${17.5 \leq I_{AB}\leq 23.5}$ . This sample, including flags 2, 3, 4 and 9, is 85% complete. The median redshift is z=0.70 and the mean redshift is z=0.80.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig25.ps} \end{figure}$ Figure 25: Same as Fig. 22 for 9141 galaxies with $17.5 \leq I_{AB} \leq 24$ . This sample, including flags 2, 3, 4 and 9, is 78% complete. The median redshift is z=0.76 and the mean redshift is z=0.90.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig26.ps} \end{figure}$ Figure 26: Redshift distribution for galaxies in the VVDS-02h field with $0 \leq z \leq 1.7$ , for galaxies with redshift quality flags 2, 3, 4, 9 (solid histogram) and galaxies with redshift quality flag 1 (dashed histogram). The redshift bin is dz=0.0033.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1960fig2.ps} \end{figure}$	Figure 2: Distribution of slit length in 6 of the VVDS-02h pointings.
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$\begin{figure} \par\includegraphics[width=15.3cm,clip]{1960fig3.ps} \end{figure}$	Figure 3: Typical layout of spectra in the 4 quadrants of a VVDS-Wide pointing; more than 550 are observed on average.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig4.ps} \end{figure}$	Figure 4: Difference between the photometric I band magnitude and the I-band magnitude computed from $\sim$ 1000 calibrated VVDS spectra. The difference is mainly due to slit losses; no systematic effect in the spectrophotometric calibration is observed vs. magnitude.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig5.ps} \end{figure}$	Figure 5: Flux-calibrated VVDS spectra compared to the photometry of the VVDS imaging survey after scaling to match to the I band flux (black dots). The spectrophotometric accuracy is conserved over the full wavelength coverage at the 10% level.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig6.ps} \end{figure}$	Figure 6: S/N per spectral resolution element over the magnitude range of the VVDS-Deep survey.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1960fig7.ps} \end{figure}$	Figure 7: Spectrum of an absorption line galaxy with I_AB=23.61, and z=3.2950, demonstrating the ability of low spectral resolution $R\sim 230$ to measure redshifts from absorption line galaxies down to the very faint end of the survey.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{1960fig8.ps} \end{figure}$	Figure 8: Redshift distribution of flag 2 objects (dashed), compared to the normalized redshift distribution of the flag 3 and 4 objects (open).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig9.ps} \end{figure}$	Figure 9: Redshift distribution of flag 1 objects (dashed), compared to the normalized redshift distribution of the flag 2, 3 and 4 objects (open).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig12.ps} \end{figure}$	Figure 12: Distribution of galaxies observed in VVDS-02h.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig13.ps} \end{figure}$	Figure 13: Number and fraction of objects observed in the VVDS-02h, compared to the total number of objects in the photometric catalog with $17.5 \leq I_{AB} \leq 24$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig14.ps} \end{figure}$	Figure 14: Difference in redshift measurements for 266 galaxies observed twice in the VVDS-02h and 139 galaxies observed twice in the VVDS-CDFS. The difference has a Gaussian distribution with $\sigma _z=13 \times 10^{-4}$ or 390 km s^-1, hence each single redshift measurement has an accuracy 390/(2)^0.5 or 276 km s^-1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig15.ps} \end{figure}$	Figure 15: Difference in redshift measurements for 33 objects in common between the VVDS-CDFS sample and the FORS2-GOODS observations of Vanzela et al. (2004). The difference has a mean d $z=8.4\times 10^{-4}$ and a $\sigma _z=12.6 \times 10^{-4}$ or 378 km s^-1.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig17.ps} \end{figure}$	Figure 17: VVDS spectra in the range $0 < z \leq 0.7$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig18.ps} \end{figure}$	Figure 18: VVDS spectra in the range $0.7 < z \leq 1.3$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1960fig19.ps} \end{figure}$	Figure 19: VVDS spectra in the range $1.3 < z \leq 2.2$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1960fig20.ps} \end{figure}$	Figure 20: VVDS spectra in the range $2.2 < z \leq 5$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig23.ps} \end{figure}$	Figure 23: Same as Fig. 22 for 5124 galaxies with $17.5 \leq I_{AB}\leq 23$ . This sample, including flags 2, 3, 4 and 9, is 90% complete. The median redshift is z=0.67 and the mean redshift is z=0.72.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig24.ps} \end{figure}$	Figure 24: Same as Fig. 22 for 7054 galaxies with ${17.5 \leq I_{AB}\leq 23.5}$ . This sample, including flags 2, 3, 4 and 9, is 85% complete. The median redshift is z=0.70 and the mean redshift is z=0.80.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig25.ps} \end{figure}$	Figure 25: Same as Fig. 22 for 9141 galaxies with $17.5 \leq I_{AB} \leq 24$ . This sample, including flags 2, 3, 4 and 9, is 78% complete. The median redshift is z=0.76 and the mean redshift is z=0.90.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1960fig26.ps} \end{figure}$	Figure 26: Redshift distribution for galaxies in the VVDS-02h field with $0 \leq z \leq 1.7$ , for galaxies with redshift quality flags 2, 3, 4, 9 (solid histogram) and galaxies with redshift quality flag 1 (dashed histogram). The redshift bin is dz=0.0033.
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