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Early Results from the VIMOS VLT Deep Survey

Published online by Cambridge University Press:  23 September 2016

O. Le Fèvre ,
C. Adami ,
O. Ilbert ,
V. Le Brun ,
C. Marinoni ,
A. Mazure ,
B. Meneux ,
S. Paltani ,
L. Tresse  and
G. Vettolani
...Show all authors
O. Le Fèvre
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
C. Adami
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
O. Ilbert
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
V. Le Brun
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
C. Marinoni
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
A. Mazure
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
B. Meneux
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
S. Paltani
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
L. Tresse
Affiliation:
Laboratoire d'Astrophysique de Marseille, France
G. Vettolani
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
M. Bondi
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
A. Cappi
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
P. Ciliegi
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
B. Marano
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
H. J. McCracken
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
L. Pozzetti
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
A. Zanichelli
Affiliation:
Istituto di Radio-Astronomia, CNR, Bologna, Italy
D. MaCcagni
Affiliation:
IASF, INAF, Milano, Italy
D. Bottini
Affiliation:
IASF, INAF, Milano, Italy
S. Foucaud
Affiliation:
IASF, INAF, Milano, Italy
P. Franzetti
Affiliation:
IASF, INAF, Milano, Italy
B. Garilli
Affiliation:
IASF, INAF, Milano, Italy
M. Scodeggio
Affiliation:
IASF, INAF, Milano, Italy
J. P. Picat
Affiliation:
Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées
T. Contini
Affiliation:
Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées
I. Gavignaud
Affiliation:
Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées
G. Mathez
Affiliation:
Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées
R. Pellò
Affiliation:
Laboratoire d'Astrophysique, Observatoire Midi-Pyrénées
M. Arnaboldi
Affiliation:
Osservatorio Astronomico di Capodimonte, Naples, Italy
G. Busarello
Affiliation:
Osservatorio Astronomico di Capodimonte, Naples, Italy
P. Merluzzi
Affiliation:
Osservatorio Astronomico di Capodimonte, Naples, Italy
M. Radovich
Affiliation:
Osservatorio Astronomico di Capodimonte, Naples, Italy
Y. Mellier
Affiliation:
Institut d'Astrophysique de Paris, Paris, France
S. Charlot
Affiliation:
Max Planck fur Astrophysik, Garching, Germany
L. Guzzo
Affiliation:
Osservatorio Astronomico di Brera, Milan, Italy
A. Iovino
Affiliation:
Osservatorio Astronomico di Brera, Milan, Italy
A. Pollo
Affiliation:
Osservatorio Astronomico di Brera, Milan, Italy
D. Rizzo
Affiliation:
Osservatorio Astronomico di Brera, Milan, Italy
R. Scaramella
Affiliation:
Osservatorio Astronomico di Roma, Italy
S. Bardelli
Affiliation:
Osservatorio Astronomico di Bologna, Bologna, Italy
M. Bolzonelle
Affiliation:
Osservatorio Astronomico di Bologna, Bologna, Italy
G. Zamorani
Affiliation:
Osservatorio Astronomico di Bologna, Bologna, Italy
E. Zucca
Affiliation:
Osservatorio Astronomico di Bologna, Bologna, Italy

Abstract

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The VIMOS VLT Deep Survey (VVDS) is underway to study the evolution of galaxies, large scale structures and AGNs, from the measurement of more than 100 000 spectra of faint objects. We present here the results from the first epoch observations of more than 20000 spectra. The main challenge of the program, the redshift measurements, is described, in particular entering the “redshift desert” in the range 1.5 < z < 3 for which only very weak features are detected in the observed wavelength range. The redshift distribution of a magnitude limited sample brighter than IAB = 24 is presented for the first time, showing a peak at a low redshift z ∼ 0.7, and a tail extending all the way above z = 4. The evolution of the luminosity function out to z = 1.5 is presented, with the LF of blue star forming galaxies carrying most of the evolution, with L* changing by more than two magnitudes for this sub-sample.

Type
Session VII: Ongoing and Future Studies
Information
Symposium - International Astronomical Union , Volume 216: Maps of the Cosmos , 2005 , pp. 381 - 389
Copyright
Copyright © Astronomical Society of the Pacific 2005 

References

Bondi, M., et al. 2003, A&A, 403, 857 Google Scholar
Le Fèvre, O., et al. 2001, in ESO Astrophysics Symposia Series, Deep Fields, ed. Cristiani, S., Renzini, A., Williams, R. E. (Berlin: Springer-Verlag), 231 Google Scholar
Le Fèvre, O., et al., 2004, A&A, 417, 839 Google Scholar