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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2008

Clustering properties of a type-selected volume-limited sample of galaxies in the CFHTLS

Résumé

We present an investigation of the clustering of the faint (i'AB<24.5) field galaxy population in the redshift range 0.2w and slope δ of the galaxy correlation function w on absolute MB rest-frame luminosity, redshift, and best-fitting spectral type (or, equivalently, rest-frame colour). Our derived comoving correlation lengths for magnitude-limited samples are in excellent agreement with measurements made in spectroscopic surveys. Our main conclusions are as follows: 1. the comoving correlation length for all galaxies with -19-1 Mpc; 5. the relative bias between redder and bluer rest-frame populations increases gradually towards fainter magnitudes. Among the most important implications of these results is that although the full galaxy population traces the underlying dark matter distribution quite well (and is therefore quite weakly biased), redder, older galaxies have clustering lengths that are almost invariant with redshift are quite strongly biased by z∼1.

Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT)

which is operated by the National Research Council (NRC) of Canada,

the Institut National des Science de l'Univers of the Centre

National de la Recherche Scientifique (CNRS) of France, and the

University of Hawaii. This work is based in part on data products

produced at TERAPIX and the Canadian Astronomy Data Centre as part

of the Canada-France-Hawaii Telescope Legacy Survey, a

collaborative project of NRC and CNRS.

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Dates et versions

hal-03646505 , version 1 (30-04-2022)

Identifiants

Citer

H. J. Mccracken, O. Ilbert, Y. Mellier, E. Bertin, L. Guzzo, et al.. Clustering properties of a type-selected volume-limited sample of galaxies in the CFHTLS. Astronomy and Astrophysics - A&A, 2008, 479, pp.321-334. ⟨10.1051/0004-6361:20078636⟩. ⟨hal-03646505⟩
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