# The VIMOS VLT Deep Survey

O. Le Fèvre, G. Vettolani, S. Paltani, L. Tresse, G. Zamorani, V. Le Brun, C. Moreau, D. Bottini, D. Maccagni, J. Picat, et al.

► To cite this version:

O. Le Fèvre, G. Vettolani, S. Paltani, L. Tresse, G. Zamorani, et al., The VIMOS VLT Deep Survey. Astronomy & Astrophysics - A&A, 2004, 428 (3), pp.1043-1049. 10.1051/0004-6361:20048072. hal-05358181

HAL Id: hal-05358181

https://hal.science/hal-05358181v1

Submitted on 11 Nov 2025

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
# The VIMOS VLT Deep Survey

## Public release of 1599 redshifts to $I_{AB} \le 24$ across the Chandra Deep Field South*

O. Le Fèvre<fnref n="1" />, G. Vettolani<fnref n="2" />, S. Paltani<fnref n="1" />, L. Tresse<fnref n="1" />, G. Zamorani<fnref n="5" />, V. Le Brun<fnref n="1" />, C. Moreau<fnref n="1" />,

D. Bottini<fnref n="3" />, D. Maccagni<fnref n="3" />, J. P. Picat<fnref n="4" />, R. Scaramella<fnref n="2" />, M. Scodeggio<fnref n="3" />, A. Zanichelli<fnref n="2" />, C. Adami<fnref n="1" />, S. Arnouts<fnref n="1" />,

S. Bardelli<fnref n="5" />, M. Bolzonella<fnref n="6" />, A. Cappi<fnref n="5" />, S. Charlot<fnref n="7" />,<fnref n="10" />, T. Contini<fnref n="4" />, S. Foucaud<fnref n="3" />, P. Franzetti<fnref n="3" />, B. Garilli<fnref n="3" />,

I. Gavignaud<fnref n="4" />,<fnref n="11" />, L. Guzzo<fnref n="8" />, O. Ilbert<fnref n="1" />, A. Iovino<fnref n="8" />, H. J. McCracken<fnref n="7" />,<fnref n="12" />, D. Mancini<fnref n="9" />, B. Marano<fnref n="6" />, C. Marinoni<fnref n="1" />,

G. Mathez<fnref n="4" />, A. Mazure<fnref n="1" />, B. Meneux<fnref n="1" />, R. Merighi<fnref n="5" />, R. Pellò<fnref n="4" />, A. Pollo<fnref n="8" />, L. Pozzetti<fnref n="5" />, M. Radovich<fnref n="9" />, E. Zucca<fnref n="5" />,

M. Arnaboldi<fnref n="9" />, M. Bondi<fnref n="2" />, A. Bongiorno<fnref n="6" />, G. Busarello<fnref n="9" />, P. Ciliegi<fnref n="5" />, L. Gregorini<fnref n="2" />, Y. Mellier<fnref n="7" />,<fnref n="12" />,

P. Merluzzi<fnref n="9" />, V. Ripepi<fnref n="9" />, and D. Rizzo<fnref n="4" />

Received 10 April 2004 / Accepted 6 August 2004

**Abstract.** This paper presents the VIMOS VLT Deep Survey around the Chandra Deep Field South (CDFS). We have measured 1599 new redshifts with VIMOS on the European Observatory Very Large Telescope – UT3, in an area 21 × 21.6 arcmin<fnref n="2" />, including 784 redshifts in the Hubble Space Telescope – Advanced Camera for Surveys GOODS area. 30% of all objects with $I_{AB} = 24$ have been observed independently of magnitude, indicating that the sample is purely magnitude limited. We have reached an unprecedented completeness level of 84% in terms of the ratio of secure measurements vs. observed objects, while 95% of all objects have a redshift measurement. A total of 1452 galaxies, 139 stars, 8 QSOs have a redshift identification, 141 of these being unsecure measurements. The redshift distribution down to $I_{AB} = 24$ is peaked at a median redshift $z = 0.73$, with a significant high redshift tail extending up to ~4. Several high density peaks in the distribution of galaxies are identified. In particular, the strong peak at $z = 0.735$ contains more than 130 galaxies in a velocity range ±2000 km s⁻<fnref n="1" /> distributed all across the transverse ~20 h⁻<fnref n="1" /> Mpc of the survey. We are releasing all redshifts to the community, along with the cross identification with HST-ACS GOODS sources on the CENCOS database environment http://cencosw.oamp.fr.

**Key words.** surveys – galaxies: high-redshift – galaxies: distances and redshifts – cosmology: observations – galaxies: evolution – cosmology: large scale structure of Universe

## 1. Introduction

Understanding the major steps in the evolution of galaxies still remains a major challenge to modern astrophysics. While

the general theoretical framework of the hierarchical growth of structures in the universe including the build up of galaxies is well in place (e.g. Peacock et al. 2004), at high redshifts this picture remains largely unconstrained by observations. The detailed properties of the main population of galaxies from large samples representative of the universe at various epochs

<footnote n="1">¹ Laboratoire d'Astrophysique de Marseille – UMR 6110, OAMP, Université de Provence, Traverse du Siphon-Les trois Lucs, BP 8, 13376 Marseille Cedex 12, France
e-mail: olivier.lefevre@oamp.fr</footnote>

<footnote n="2">² IRA-INAF, via Gobetti 101, 40129 Bologna, Italy</footnote>

<footnote n="3">³ IASF-INAF, via Bassini 15, 20133 Milano, Italy</footnote>

<footnote n="4">⁴ Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées – UMR 5572, 14 avenue E. Belin, 31400 Toulouse, France</footnote>

<footnote n="5">⁵ INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy</footnote>

<footnote n="6">⁶ Università di Bologna, Dipartimento di Astronomia, via Ranzani 1, 40127 Bologna, Italy</footnote>

<footnote n="7">⁷ Institut d'Astrophysique de Paris – UMR 7095, 98bis bd Arago, 75014 Paris, France</footnote>

<footnote n="8">⁸ INAF – Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy</footnote>

<footnote n="9">⁹ INAF – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy</footnote>

<footnote n="10">¹⁰ Max Planck Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany</footnote>

<footnote n="11">¹¹ European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany</footnote>

<footnote n="12">¹² Observatoire de Paris, LERMA – UMR 8112, 61 avenue de l'Observatoire, 75014 Paris, France</footnote>

<footnote>* The data presented in this paper has been obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile.</footnote>
remain to be established across most of the life of the uni-
verse beyond the large local volumes explored by the 2dFGRS
(Colless et al. 2001) and the SDSS (Schneider et al. 2003), and
expanding from smaller exploratory surveys (Lilly et al. 1995;
Le Fèvre et al. 1995; Steidel et al. 2003; Cimatti et al. 2002).

The VIMOS VLT Deep Survey (VVDS) is a deep redshift
survey aimed at studying the evolution of galaxies, large scale
structures and AGNs over more than 90% of the current age
of the universe. The unique feature of the VVDS is the sim-
ple magnitude selection applied to define a complete magni-
tude limited sample of distant galaxies, with a goal of more
than 100 000 objects observed in multi-object spectroscopy.
The VVDS rests on the observations of 5 different fields to
smooth out the effects of cosmic variance when building the
statistical properties of the galaxy population (Le Fèvre et al.
2004).

This paper presents the redshift survey observations of
1599 objects with $I_{AB} \le 24$ conducted by the VVDS team
around the Chandra Deep Field South (CDFS). The CDFS
is field particularly rich of deep observations, starting from
1 Ms Chandra observations (Giacconi et al. 2002), including
the HST-GOODS area (Giavalisco et al. 2004), as well as opti-
cal spectroscopy (Szokoly et al. 2003). The observations have
been carried out with the VISIBLE Multi-Object Spectrograph
(VIMOS) on the 8.2 m Melipal telescope of the European
Southern Observatory Very Large Telescope. We are describ-
ing the processing steps and redshift measurements, and the
associated quality control we have applied to these data. The
content of the final catalog is detailed, as well as the cross iden-
tification with the Hubble Space Telescope Advanced Camera
for Surveys GOODS images, and we present the main entries
available from our interactive database. The main properties of
the sample are briefly presented, including the redshift distri-
bution of the sample.

**2. Observations**

**2.1. Multi-Object Spectroscopy with VIMOS**

Spectroscopic observations have been conducted with VIMOS
on the VLT-UT3 Melipal (Le Fèvre et al. 2003). The low reso-
lution red grism LRRED has been used with slits of 1 arcsec
width. The spectral resolution in this mode is 34 Å at 7500 Å
or R ~ 220. The spectral length has been limited by the red
bandpass filter to 5500–9500 Å. Slits placed on objects have a
typical length ~10 arcsec each.

**2.2. VIMOS pointings**

A complete VIMOS pointing is a combination of observations
with the 4 quadrants of the instrument, each separated by a
cross about 2 arcmin wide. With the above setup and the pro-
jected sky density of objects down to $I_{AB} = 24$, one VIMOS
pointing allows to observe ~450 targets in one single observa-
tion (Le Fèvre et al. 2003).

We have set a total of 5 pointings around the Chandra
Deep Field South, the positions are listed in Table 1. Together,
they cover a total area of ~453'² including the complete

<figure><img src="image_2.png" /><figcaption>Fig. 1. Objects observed with VIMOS-VLT around the Chandra Deep Field South. Black circles are objects in the HST-ACS GOODS area.</figcaption></figure>

HST-GOODS survey field (Giavalisco et al. 2004). The layout
of observed galaxies is presented in Fig. 1.

**2.3. Mask preparation**

The preparation of slit masks for VIMOS observations has
been done using the photometric catalog produced by the ESO
Imaging Survey (EIS, Arnouts et al. 2001), and short images
taken with VIMOS. The VIMOS images are used to produce
a catalog of source positions in the VIMOS instrument coordi-
nate system, which are then cross-correlated with the EIS cat-
alog to compute the transformation matrix from the EIS cat-
alog astrometric system to the VIMOS focal plane where slit
masks are located. The VMMPS code was then run on the EIS
catalog for all sources brighter than $I_{AB} = 24$ to optimize the
number and positions of slits for each of the 4 masks per point-
ing. Masks have been cut by ESO Paranal Staff using the Mask
Manufacturing Unit (Conti et al. 2001).

**2.4. VIMOS observations**

Observations with VIMOS have been obtained between
October 31 and December 6, 2002. Observing conditions were
photometric with an image quality between 0.6 and 1.2 arcsec
FWHM. We have moved the telescope, hence the objects along
the slits, in a sequence of 5 positions with offsets -1.4, -0.7,
0, +0.7, +1.4 arcsec from the reference pointing position. This
is necessary to compute the fringing pattern produced above
8300 Å by the thinned EEV CCDs used in VIMOS, and re-
move it during processing.

Wavelength calibrations have been obtained during the day,
oberving Helium and Argon arc lamps through the observed
masks. The spectrophotometric standard star LTT3218 has
been used to derive the absolute flux calibration.
<table><caption>**Table 1.** Observed VIMOS pointings.</caption><thead><tr><th>Pointing<br>VVDS</th><th>α<sub>2000</sub><br>(2000)</th><th>δ<sub>2000</sub><br>(2000)</th><th>Date<br>Observed</th><th>Number<br>of slits</th><th>T<sub>exp</sub><br>min</th></tr></thead><tbody><tr><td>CDFS001</td><td>03h32m28.0s</td><td>-27°48'30"</td><td>31-Oct-02<br>1, 2, 4-Nov.-02</td><td>447</td><td>10 × 27</td></tr><tr><td>CDFS002</td><td>03h32m37.04s</td><td>-27°50'30"</td><td>5, 6-Nov.-02</td><td>331<sup>a</sup></td><td>8 × 27</td></tr><tr><td>CDFS003</td><td>03h32m18.95s</td><td>-27°50'30"</td><td>9, 10, 11, 12-Nov.-02</td><td>447</td><td>9 × 27</td></tr><tr><td>CDFS004</td><td>03h32m37.04s</td><td>-27°46'30"</td><td>27, 28, 29-Nov.-02<br>1, 2-Dec.-02</td><td>436</td><td>12 × 27</td></tr><tr><td>CDFS005</td><td>03h32m18.95s</td><td>-27°46'30"</td><td>2,4,5,6-Dec.-02</td><td>448</td><td>10 × 27</td></tr></tbody></table>

### 3. Data Processing

Data processing has been conducted under the VIPGI environment developed by our team (Franzetti et al. 2004). VIPGI has been used to organize the multiple files and process all data from the raw 2D images and calibration to the production of sky subtracted, wavelength and flux calibrated 1D spectra. Because of instrument flexures not yet minimized at the time of these observations, the fringing pattern has been occasionally hard to remove. The quality control performed on these steps is described in Le Fèvre et al. (2004). The wavelength accuracy is better than ~1 Å rms all over the wavelength range, and the spectrophotometry is accurate to about 10%.

### 4. Redshift measurements

Measuring redshifts for a complete magnitude limited sample down to $I_{AB} = 24$ had never been attempted before our observations. The challenge is to measure redshifts over a large possible range $0 \le z \le \sim 5$, without any other a priori information than the magnitude selection. The approach we have followed involves an iterative build up of galaxy templates as observed with VIMOS, coupled to the powerful redshift measuring machine KBRED (Scaramella et al. 2004), based on cross correlation and principal component analysis methods. This approach has been applied and tuned on the more than 20 000 spectra obtained for the VVDS in the fall of 2002, and remained until recently very manpower intensive. On this critical step, we have enforced a very strict quality control.

Each spectrum has been measured independently by 2 VVDS team members, and then compared. A final check has been done by a third team member prior to release into the database. Each spectrum is assigned a redshift, and a flag indicating the reliability level of the measurement, as defined in Le Fèvre et al. (1995) and described in Sect. 6. Flags 2, 3, 4 are the most secure, flag 1 is an indicative measurement based on continuum and few supporting features, and flag 0 indicates a measurement failure with no features identified. Flag 9 indicates that there is only one secure emission line tentatively assigned to the listed redshift (e.g. [OII]3727 Å or $H\alpha$).

<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Redshift difference between objects observed twice or more in independent VIMOS observations. The distribution has a velocity dispersion $\sigma_z = 0.0012$ or $360 \text{ km s}^{-1}$, hence the accuracy in redshift measurement is $360/\sqrt{2} \sim 255 \text{ km s}^{-1}$.</figcaption></figure>

#### 4.1. Redshift accuracy

The redshift accuracy can be estimated from a sample of 160 galaxies which have been observed twice with VIMOS within the 5 CDFS pointings. These galaxies have been included in two or more different mask sets, and observed independently at different times. The distribution of measured redshift differences is presented in Fig. 2. The dispersion of the redshift difference distribution is $\sigma = 0.0012$, or $360 \text{ km s}^{-1}$, hence the accuracy of a single redshift measurement is $360/\sqrt{2} \sim 255 \text{ km s}^{-1}$.

We have compared our redshift measurements with the measurements of the K20 survey (Cimatti et al. 2002) and VLT-FORS2 measurements conducted by the ESO-GOODS team (www.eso.org/science/goods). A total of 70 objects have been observed both by the VVDS and the K20. For the 63 VVDS objects with flags $\ge 1$, the redshifts agree for ~87% of the sample with a $\Delta z = -0.0004$ and $\sigma_z = 0.0017$, with the main disagreement concentrated on flag 1, as expected.

<footnote>a Quadrant 2 not observed.</footnote>
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Completeness of the $I_{AB} \le 24$ sample. (Top panel) the fraction of secure redshift measurements and all measurements. The overall redshift measurement completeness is 84% with redshift measurements for 95% of the sample. (Middle panel) The magnitude distribution of galaxies with secure redshift measurements (open histogram), and failed measurements (filled histogram). See text for the statistical computation of the failed measurements. (Lower panels) magnitude distribution of the galaxies for each of the quality flags.</figcaption></figure>

The comparison with the ESO-GOODS data yields 46 objects in common, of which 42 have a VVDS flag $\ge 1$. TheVVDS vs. ESO-GOODS redshifts agree for 66% of the sample with $\Delta z = -0.0006$ and $\sigma_z = 0.0013$. There are 48 objects in common between our observation an the observations of X-ray sources by Szokoly et al. (2003), and our redshifts agree on 85% of this special class of objects (Hasinger, private communication). The detailed comparison of VVDS redshift measurements with the measurements from these other teams will be presented in Le Fèvre et al. (2004).

## 4.2. Completeness

We have defined the completeness of the measurements as the ratio between the actual redshifts measurements and the observed spectra. We have removed from the list of observed spectra those which have a clearly identified instrumental or data processing problem affecting the measurement, like e.g. the slit is behind the guide probe of the VLT-UT3, or the data processing with VIPGI failed to properly detect the object because of strong residual features from the sky/fringing corrections. This will be described in details in Le Fèvre et al. (2004).

We are presenting in Fig. 3 the completeness in redshift measurement vs. $I_{AB}$ magnitude for all objects (galaxies, stars, QSOs), and the magnitude distribution of objects with flags 0, 1, 2, 3, 4, 9. The completeness is computed taking into account the fraction of objects with a good redshift measurement

<figure><img src="image_5.png" /><figcaption>**Fig. 4.** (Top panel) $I_{AB}$ magnitude distribution of objects observed with VIMOS in the Chandra Deep Field South (filled histogram), compared to the distribution of all objects in the area in the EIS photometric catalog (open histogram). (Bottom panel) The ratio of observed vs. all objects is 0.3.</figcaption></figure>

for each of our quality flags listed in Sect. 7 (see Le Fèvre et al. 2004 for a detailed discussion on completeness).

The overall redshift measurement completeness reaches 84%. The objects with a redshift measurement listed in the catalogs, flags 1, 2, 3, 4, 9, 11, 12, 13, 14, 19, represent 95% of the sample, excluding objects with flags 0.

# 5. Cross identification with HST-ACS GOODS sources

The cross identification of the objects observed from the EIS catalog and the objects detected by HST-ACS has been performed running a cross correlation of our target list with the list of objects published in the version r1.0, December 22, 2003, of the GOODS survey multi-band catalog. The relative astrometry of the EIS vs. GOODS catalogs has been found to be extremely good, to within 0.1 arcsec over our survey field. A search circle with radius 0.3 arcsec has been used to search for HST sources corresponding to the ground based sources. This produced a matched list with only one to one identifications, and no double identifications.

# 6. Basic properties of the sample

## 6.1. Magnitude distribution

The magnitude distribution of objects observed in our survey is shown in Fig. 4 compared to the distribution of all objects in the EIS photometric catalog over the same area. We have observed 30% of all objects with $I_{AB} \le 24$ in the area covered by the survey, independently of magnitude, as shown in Fig. 4. This demonstrates that there is no magnitude-dependent bias in our object selection and that our sample is purely magnitude
<figure><img src="image_6.png" /></figure>

**Fig. 5.** Redshift distribution of galaxies with $I_{AB} \le 24$ observed with VIMOS in the Chandra Deep Field South. The redshift bin is $dz = 0.005$. There are 42 objects identified with $z \ge 2$ not included in this figure.

selected even after the complex target selection in the making of the VIMOS multi-slit masks.

## 6.2. Redshift distribution

The redshift distribution (up to $z = 2$) of the full sample of galaxies and QSOs is presented in Fig. 5. The median of the redshift distribution is $\langle z \rangle = 0.73$. Galaxies are identified up to $z = 4.63$. As described in Le Fèvre et al. (2004) and Paltani et al. 2004, we have been successful in breaking into the “redshift desert” artificially produced by the difficulty to identify redshifts in the range $1.5 \le z \le 3$ due to our instrumental set-up, through extensive work on galaxy templates based on the high redshift galaxies measured in the VVDS (Paltani et al. 2004). We extensively discuss the incompleteness of the VVDS sample vs. redshift in Le Fèvre et al. (2004).

The strongest peaks in the distribution are at redshifts $z = 0.667$, and $z = 0.735$, confirming with better statistics the observations of Gilli et al. (2003). A total of 149 galaxies are measured in the $z = 0.667$ peak and 116 galaxies $z = 0.735$ peak. These structures are extending all across transverse ~16 Mpc of this survey ($z \sim 0.7$ ΛCDM with $H_0 = 70$, $\Omega_m = 0.3$, $\Omega_{\text{Lambda}} = 0.7$) in a wall-like pattern rather than in clusters. These peaks are also traced by X-ray sources as discussed by Szokoly et al. (2003).

## 6.3. Absolute magnitude and B−I distributions vs. redshift

The absolute magnitude $M_B$ vs. redshift distribution is presented in Fig. 6. The absolute magnitudes have been computed based on $k(z)$ corrections derived from the fitting of the broad band photometry using rest frame galaxy templates

<figure><img src="image_7.png" /></figure>

**Fig. 6.** Absolute $M_{B_{AB}}$ magnitude – redshift distribution for the full VVDS–CDFS sample

<figure><img src="image_8.png" /></figure>

**Fig. 7.** $B_{AB} - I_{AB}$ vs. redshift distribution for the full VVDS–CDFS sample

(see Ilbert et al. 2004). The $B_{AB} - I_{AB}$ vs. redshift distribution is presented in Fig. 7

# 7. The CDFS catalog

Our catalog contains 1599 spectra including 1452 galaxies, 139 stars, and 8 QSOs. We have listed for each observed object:

- the ESO Imaging Survey identification number, equatorial coordinates $\alpha_{2000}$, $\delta_{2000}$, $I_{AB}$ magnitudes and associated errors (Arnouts et al. 2001);

- the HST-GOODS identification number and $BVI_z$ magnitudes and associated errors (Giavalisco et al. 2004);
<figure><img src="image_9.png" /><figcaption>**Fig. 8.** Output from the VVDS-CDFS CENCOS database output panel for one single object. All information is presented, including the EIS and HST-GOODS identifiers, the ground based and HST-ACS magnitudes, the VVDS redshift and quality flag, and the HST-GOODS images and VVDS spectrum are displayed.</figcaption></figure>

- the redshift measured by the VVDS team;

- the redshift quality flag (see Le Fèvre et al. 2004, for a detailed description). The flags definition taken from the Canada France Redshift Survey (Le Fèvre et al. 1995) is as follows:

0: no redshift could be measured;

1: some spectral features like e.g. weak line(s) or continuum break give a possible indication of the redshift (50–55%; of the redshifts are correct);

2: a few secure features are identified in support of the redshift measurement (80–85% of the redshifts are correct);

3: many secure features are identified (93–96% of the redshifts are correct);

4: strong secure features with high S/N are identified (98–99% of the redshifts are correct);

5: one secure emission line tentatively assigned to the listed redshift (e.g. [OII]3727 Å or H$\alpha$).

## 8. Public data release

We are publicly releasing all redshift measurements through the CENCOS (CENtre de COSmologie) database environment on our web site http://cencosw.oamp.fr with access to the database built under the Oracle environment. The catalog can be searched by coordinates, redshift interval, identification

number in the EIS or GOODS catalogs, in combination with the spectra quality flags. Upon query, the database engine returns a list of targets, each of them can be examined in one single summary panel with all the VVDS spectroscopy information including the spectra, as well as the EIS and B, V, I, z HST-GOODS images, and associated photometry as shown in Fig. 8.

## 9. Summary

In the framework of the VIMOS VLT Deep Survey (VVDS), we have observed a large sample of galaxies around the Chandra Deep Field South, and are releasing the redshift data to the community. A total of 1599 objects with $I_{AB} \le 24$ have a measured redshift. The completeness in redshift measurement for the targeted objects is high, above 84%. We find that the redshift distribution has a median of $z = 0.73$, with strong high density peaks observed across the field.

The combination of this redshift survey and the HST-ACS GOODS survey enables detailed studies of the evolution of galaxies in the Chandra Deep Field South.

**Acknowledgements.** We are grateful to A. Cimatti and the K20 team for releasing their redshift measurements to us for comparison, and we thank G. Hasinger for communicating to us a comparison with
the Szokoly et al. spectroscopy. The VLT-VIMOS observations have been carried out on guaranteed time (GTO) allocated by the European Southern Observatory to the VIRMOS consortium, under a contractual agreement between the Centre National de la Recherche Scientifique of France, heading a consortium of French and Italian institutes, and ESO, to design, manufacture and test the VIMOS instrument.

## References

* Arnouts, S., Vandame, B., Benoist, C., et al. 2001, A&A, 379, 740

* Cimatti, A., Daddi, E., Mignoli, M., et al. 2002, A&A, 381, L68

* Colless, M. M., Dalton, G., Maddox, S., et al. 2001, MNRAS, 328, 1039

* Conti, G., Mattaini, E., Maccagni, D., et al. 2001, PASP, 113, 452

* Franzetti, P., Scoddegio, M., & the VVDS team 2004, A&A, in preparation

* Giacconi, R., Zirm, A., Wang, J., et al. 2002, ApJS, 139, 369

* Giavalisco, M., & GOODS team 2004, ApJ, 600, L93

* Gilli, R., Cimati, A., Daddi, E., et al. 2003, ApJ, 592, 721

* Ilbert, O., & the VVDS team, A&A, submitted

* Le Fèvre, O., Crampton, D., Lilly, S. J., Hammer, F., & Tresse, L. 1995, ApJ, 455, 60

* Le Fèvre, O., & the VVDS team 2003, The Messenger 111, 18

* Le Fèvre, O., & the VVDS team 2004, A&A, submitted

* Lilly, S. J., Le Fèvre, O., Crampton, D., Hammer, F., & Tresse, L. 1995, ApJ, 455, 50

* Paltani, S., & the VVDS team 2004, in preparation

* Peacock, J. 2002 Tenerife Winter School, Dark matter and dark energy in the universe [arXiv:astro-ph/0309240]

* Scaramella, R., & the VVDS team 2004, in preparation

* Steidel, C. C., Adelberger, K. L., Shapley, A. E., et al. 2003, ApJ, 592, 728

* Schneider, D. P., Fan, X., Hall, P. B., et al. 2003, AJ, 126, 2579

* Szokoly, G. P., Bergeron, J., Hasinger, G., et al. AJ, submitted, [arXiv:astro-ph/0312324]