The VIMOS VLT Deep Survey (VVDS)

Latest News 2008, January
A test of the nature of cosmic acceleration using galaxy redshift distorsions

The active VVDS Team
  • PI: O. Le Fèvre (LAM)
  • Builders: B. Garilli (INAF-IASF), V. Le Brun (LAM), D. Maccagni (INAF-IASF), M. Scodeggio (INAF-IASF), L. Tresse (LAM), A. Zanichelli (INAF-IRA)
  • Survey Core: C. Adami, S. Arnouts, S. Bardelli, M. Bolzonella, A. Cappi, S. Charlot, P. Ciliegi, T. Contini, O. Cucciati, P. Franzetti, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, H.J. McCracken, C. Marinoni, A. Mazure, B. Meneux, S. Paltani, A. Pollo, L. Pozzetti, M. Radovich, L. Ravel, S. de la Torre, D. Vergani, G. Zamorani, E. Zucca
  • Associates: M. Bondi, J. Blaizot, A. Bongiorno, L. Gregorini, E. Perez-Montero
  • Previous co-PI / Builders / Members / Associates G. Vettolani (INAF-IRA) / D. Bottini (INAF-IASF), J.P. Picat (LAOMP), R. Scaramella (INAF-OAR) / M. Arnaboldi, G. Busarello, S. Foucaud, F. Lamareille, G. Mathez, B. Marano, Y. Mellier, R. Merighi, P. Merluzzi, R. Pello / J. Brinchmann, S. Gwyn, D. Rizzo, S. Temporin, C.J. Walcher

Astrometry/Photometry Spectroscopy Simulation
Click on the images to get full-sized images
Composite VVDS BVRIK image, 150 arcmin². Noise-normalized sum of (B+V) (blue pixels), (R+I) (green pixels) and K (red pixels) images. Integration times were 6-7 hrs in each optical bands, and 1-2hrs in K. Objects as faint as B~26 magnitude are easily visible. Courtesy McCracken for the VVDS and TERAPIX consortia.
VIMOS simulated spectra, one of 4 quadrants of 7'x8'. Courtesy Le Fevre, Tresse, Charlot for the VVDS consortium.
VVDS survey cone simulation from z=0 (bottom-right) to z=5 (top-left). Courtesy Colombi et al., IAP.


SURVEY LAYOUT (as defined in 1996)

The VIRMOS VLT Deep Survey (note that the VVDS stands for VIMOS VLT Deep Survey since the IR MOS, NIRMOS, has been turned down by ESO in 2001) is a breakthrough spectroscopic survey which will provide a complete picture of galaxy and structure formation over a very broad redshift range (0 < z < 5) over sixteen square degrees of the sky in four separate fields. This ambitious survey is possible thanks to the impressive multiplex gains of the VIRMOS instruments (VIMOS and NIRMOS) built by the Franco-Italian VIRMOS consortium for ESO-VLT. The survey will be carried out over the consortium's 120 nights of guaranteed time (note that the actual number of garanteed nights have been lowered to 60 nights by ESO in 2001), and will contain in total a sample of 150,000 spectroscopic redshifts. This unique data set will enable us to trace back the evolution of galaxies, active galactic nuclei and clusters to epochs where the Universe was a fraction (about 20 per cent) of its current age. The VVDS will be comparable in size to the largest redshift surveys currently underway in the nearby Universe, but will probe to much higher redshifts. It will provide an unparalleled description of how structures and galaxy populations evolved in the Universe from high redshift to the present day.

Strategy

The survey is conducted in two main steps: the Imaging survey and the Spectroscopic survey. The deep imaging is to obtain UBVRI over 16 deg² and K' imaging over selected areas, with the CFHT, ESO-NTT and ESO-2.2m. The VLT VIMOS and NIRMOS will allow to measure redshifts from magnitude selected samples of galaxies picked from the imaging survey.

Survey Output

We will use the survey for a number of fundamental questions in modern observational cosmology to:
The output from the survey is expected to set major constraints onto galaxy formation models, large scale structure formation models, and cosmological scenarii describing the evolution of the Universe.

Imaging Survey

Imaging Survey Overview

The VVDS is imaged in using the CFHT-CFH12K camera (BVRI filters), the ESO-NTT-SOFI (K' filter), and the ESO-2.2m-WFI (U filter). Data pipelines and processing have been developed by the TERAPIX consortium. Processing of the UBVRI imaging data has been carried at the TERAPIX facility, which provides catalogues of calibrated images of all VVDS fields. The infrared data (K') has been processed independantly by the VIRMOS consortium. Photometric catalogues are provided in using SExtractor.

Shallow Survey: 4 areas, 2x2 deg² each in UBVRIK'

Deep Survey: 1 area on 0226-0430, 2 deg² in UBVRIK'

UBVRIK' Imaging Survey Definition Parameters

Filter Telescope
Instrument
Sensitivity AB mag.
3 sigma detection of extended object in a 3 arcsecond aperture / stellar source
Field to be covered
(deg²)
Exposure time
(minutes)
Survey Status Publications
U
shallow
ESO-2.2m
WFI
24.5 / 25.71650VVDS-U survey
(www public)
Radovich et al., 2004, AA, 417, 51
U
deep
ESO-2.2m
WFI
26.0 / 27.22780VVDS-U survey
(www public)
Radovich et al., 2004, AA, 417, 51
B
shallow
CFHT
12K
25.7 / 26.816120VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
B
deep
CFHT
12K
26.5 / 27.72600VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
V
shallow
CFHT
12K
25.4 / 26.21690VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
V
deep
CFHT
12K
26.0 / 27.22270VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
R
shallow
CFH|T
12K
25.4 / 26.21660VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
R
deep
CFHT
12K
26.0 / 27.22180VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
I
shallow
CFHT
12K
24.8 / 26.01660VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
I
deep
CFHT
12K
25.4 / 26.62180VVDS-BVRI survey
(www public)
Le Fèvre , 2004, AA, 417, 839
JESO-NTT
SOFI
    VVDS-NIR survey
(restricted access)
Iovino et al., 2005, AA, 442, 423
K'
deep
ESO-NTT
SOFI
21.5 / 22.70.25180VVDS-NIR survey
(restricted access)
Iovino et al., 2005, AA, 442, 423

Other Multi-Wavelength coverage over VVDS deep field 0226-0430

  • VVDS-RADIO survey, 1.4GHz-VLA and 0.610GHz-GMRT (restricted access and public access)

  • CFHLS/D1 data, u*g'r'i'z'-CFHT/Megacam (public access)

  • GALEX data, FUV-1500 and NUV-2300

  • SPITZER/SWIRE data, IRAC-3.6,4.5,5.8,8 and MIPS-24,70,170

  • XMDS data

  • UKDISS/DES survey, data in J, H, K


  • Spectroscopic Survey

    The VVDS Spectroscopic Fields

    • Shallow Data
    • Field Alpha (2000) Delta (2000) Field size L, b Spectroscopic Survey
      0226-0430 02:26:00 -04:30:00 2x2 deg² 172.0d, -58.0d IAB=22.5
      (12K data)
      0332-2748
      (aka CDFS)
      03:32:28 -27:48:30 2x1 deg²   IAB=22.5
      (EIS data)
      1003+0154 10:03:39 01:54:39 2x2 deg² 237.8d, +42.6d IAB=22.5
      (12K data)
      1400+0500 14:00:00 05:00:00 2x2 deg² 342.4d, +62.5d IAB=22.5
      (12K data)
      2217+0024 22:17:51 00:24:27 2x2 deg² 63.3d, -44.0d IAB=22.5
      (12K data)


    • Deep Data
    • Field Alpha (2000) Delta (2000) Field size L, b Spectroscopic Survey
      0226-0430 02:26:00 -04:30:00 1x2 deg² 172.0d, -58.0d IAB=24.0
      (12K data)
      0332-2748
      (aka CDFS)
      03:32:28 -27:48:30 2x1 deg²   IAB=24.0
      (EIS data)


    • Ultra Deep Data
    • Field Alpha (2000) Delta (2000) Field size L, b Spectroscopic Survey
      0226-0430 02:26:00 -04:30:00 1x2 deg² 172.0d, -58.0d IAB=24.75
      (12K data)

    Laurence.Tresse AT oamp.fr
    Last modified: Thur Jan 31 16:59:53 CET 2008