The VIMOS VLT Deep Survey: the redshift distribution N(z) of magnitude-limited samples down to iAB=24.75 and KsAB=22

Дата и время публикации : 2013-07-24T18:28:07Z

Авторы публикации и институты :
O. Le Fevre (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
P. Cassata (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
O. Cucciati (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
S. de la Torre (SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UK)
B. Garilli (INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, Milano, Italy)
O. Ilbert (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
V. Le Brun (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
D. Maccagni (INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, Milano, Italy)
L. Tresse (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
G. Zamorani (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
S. Bardelli (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
M. Bolzonella (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
T. Contini (Institut de Recherche en Astrophysique et Planetologie, IRAP, Universite de Toulouse, UPS-OMP, Toulouse, France)
A. Iovino (INAF – Osservatorio Astronomico di Brera, Milano, Italy)
C. Lopez-Sanjuan (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France, Centro de Estudios de Fisica del Cosmos de Aragon, Teruel, Spain)
H. J. McCracken (Institut d’Astrophysique de Paris, CNRS, Universite Pierre et Marie Curie, Paris, France)
A. Pollo (Astronomical Observatory of the Jagiellonian University, Cracow, Poland, National Centre for Nuclear Research, Warszawa, Poland)
L. Pozzetti (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
M. Scodeggio (INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, Milano, Italy)
L. Tasca (Aix-Marseille Universite, CNRS, LAM – Laboratoire d’Astrophysique de Marseille, Marseille, France)
D. Vergani (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)
A. Zanichelli (INAF – Istituto di Radioastronomia, Bologna, Italy)
E. Zucca (INAF – Osservatorio Astronomico di Bologna, Bologna, Italy)

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: Submitted to Astronomy and Astrophysics
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: We measure and analyse the redshift distribution N(z) of magnitude-selected samples using spectroscopic redshift measurement from the magnitude-selected VIMOS VLT Deep Survey (VVDS) with 17<iAB<24.75. We compute the N(z) and provide reference parametric fits for i band, J, H and Ks band magnitud limited samples. The N(z) of a sample with iAB<24 has a mean redshift z=0.92, with 8.2% of the galaxies with z>2. Down to iAB<24.75 the sample has a mean redshift z=1.15 and 17.1% of the galaxies are beyond z=2. The projected sky density is 2.07+/-0.12 gal/arcmin2 at 1.4<z<2.5 and KsAB<22.5, 1.72+/-0.15 gal/arcmin2 at 2.7<z<3.4 and 0.59+/-0.09 gal/arcmin2 at 3.4<z<4.5 brighter than iAB=24.75. Galaxies at z~3 identified from magnitude-selected samples are 1.5 to 3 times more numerous than when they are colour-colour selected. We demonstrate that colour-colour selected samples over 1.4<z<4.5 are strongly contaminated by galaxies at other redshifts. Semi-analytic models on the Millennium simulations under-predict the number of luminous star-forming galaxies at zsim1.8-2, as well as over-predict the number of low-luminosity galaxies at z<0.8. Our study provides comprehensive galaxy number counts N(z) from galaxies with spectroscopic redshifts over a large redshift domain 0<z<5, a solid basis for the measurement of volume-complete quantities. Magnitude-selected surveys identify a higher number of galaxies at z>2 than in colour-colour selected samples, and we use the magnitude-selected VVDS to emphasize the large uncertainties associated to other surveys using colour or colour-colour selected samples. Our results further demonstrate that semi-analytical models on dark matter simulations have yet to find the right balance of physical processes and time-scales to properly reproduce a fundamental galaxy population property like the observed N(z).

Category: Physics