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The VIMOS VLT Deep Survey (VVDS)

  • R. Pelló
  • O. Le Fèvre
  • C. Adami
  • M. Arnaboldi
  • S. Arnouts
  • S. Bardelli
  • M. Bolzonella
  • A. Bongiorno
  • M. Bondi
  • D. Bottini
  • G. Busarello
  • A. Cappi
  • S. Charlot
  • P. Ciliegi
  • T. Contini
  • S. Foucaud
  • P. Franzetti
  • B. Garilli
  • I. Gavignaud
  • L. Guzzo
  • O. Ilbert
  • A. Iovino
  • F. Lamareille
  • V. Le Brun
  • D. Maccagni
  • B. Marano
  • C. Marinoni
  • G. Mathez
  • A. Mazure
  • H. J. McCracken
  • Y. Mellier
  • B. Meneux
  • P. Merluzzi
  • R. Merighi
  • S. Paltani
  • J. P. Picat
  • A. Pollo
  • L. Pozzetti
  • M. Radovich
  • V. Ripepi
  • D. Rizzo
  • R. Scaramella
  • M. Scodeggio
  • L. Tresse
  • G. Vettolani
  • A. Zanichelli
  • G. Zamorani
  • E. Zucca
Conference paper

This paper1 reviews the main results obtained so far by the VIRMOS VLT Deep Survey (VVDS) collaboration. The VVDS is one of the leading extragalactic surveys, started in 2002 using GTO awarded for the construction of VIMOS-VLT. Its aim is to study the evolution of galaxies, large-scale structures, and AGNs from a goal sample of 100,000 objects down to a magnitude I(AB)=24, with redshifts measured using VIMOS-VLT (typically in the range 0 < z < 5), and a wide wavelength coverage from different follow-up observations. Among the most important results achived by the VVDS so far are the redshift distributions for different galaxy populations, the evolution of the galaxy Luminosity Function in various filter bands (as a function of redshift, galaxy type, and environment), the evolution of the typedensity relation with redshfit, and the clustering properties from z 2. One of the most impressive findings of the VVDS using a pure magnitude-selected sample is the existence of an important population of bright galaxies at 1.6 < z < 5, 1.6 to 6.2 times larger than previous estimates based on color preselections (LBG technique).

Keywords

Active Galactic Nucleus Spectral Type Cosmic Time Luminosity Function Galaxy Evolution 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer 2007

Authors and Affiliations

  • R. Pelló
    • 1
  • O. Le Fèvre
    • 2
  • C. Adami
    • 2
  • M. Arnaboldi
    • 3
  • S. Arnouts
    • 2
  • S. Bardelli
    • 4
  • M. Bolzonella
    • 4
  • A. Bongiorno
    • 4
  • M. Bondi
    • 5
  • D. Bottini
    • 6
  • G. Busarello
    • 3
  • A. Cappi
    • 4
  • S. Charlot
    • 7
  • P. Ciliegi
    • 4
  • T. Contini
    • 1
  • S. Foucaud
    • 6
  • P. Franzetti
    • 6
  • B. Garilli
    • 6
  • I. Gavignaud
    • 8
  • L. Guzzo
    • 9
  • O. Ilbert
    • 4
  • A. Iovino
    • 9
  • F. Lamareille
    • 1
  • V. Le Brun
    • 2
  • D. Maccagni
    • 6
  • B. Marano
    • 4
  • C. Marinoni
    • 9
  • G. Mathez
    • 1
  • A. Mazure
    • 2
  • H. J. McCracken
    • 7
  • Y. Mellier
    • 7
  • B. Meneux
    • 2
  • P. Merluzzi
    • 3
  • R. Merighi
    • 4
  • S. Paltani
    • 2
  • J. P. Picat
    • 1
  • A. Pollo
    • 9
  • L. Pozzetti
    • 4
  • M. Radovich
    • 3
  • V. Ripepi
    • 3
  • D. Rizzo
    • 10
  • R. Scaramella
    • 5
  • M. Scodeggio
    • 6
  • L. Tresse
    • 2
  • G. Vettolani
    • 5
  • A. Zanichelli
    • 5
  • G. Zamorani
    • 4
  • E. Zucca
    • 4
  1. 1.Laboratoire d'Astrophysique, UMR 5572Observatoire Midi-PyrénéesFrance
  2. 2.Laboratoire d'Astrophysique de Marseille (UMR 6110)CNRS-Université de ProvenceFrance
  3. 3.Osservatorio Astronomico di Capodimonte INAFItaly
  4. 4.Osservatorio Astronomico di Bologna INAFItaly
  5. 5.Istituto di Radio-AstronomiaINAFItaly
  6. 6.IASFINAFItaly
  7. 7.Observatoire de ParisFrance
  8. 8.European Southern ObservatoryGermany
  9. 9.Osservatorio Astronomico di Brera INAFItaly
  10. 10.Imperial College of ScienceTechnology and MedicineLondon

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