Volume 409, Number 3, October III 2003
|Page(s)||835 - 850|
|Section||Cosmology (including clusters of galaxies)|
|Published online||17 November 2003|
The Canada-France deep fields survey–II: Lyman-break galaxies and galaxy clustering at z *
Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille Cedex 12, France
2 Present address: Istituto di Astrofisica Spaziale e Fisica cosmica – Sezione di Milano, via Bassini 15, 20133 Milano, Italy
3 Present address: University of Bologna, Department of Astronomy, via Ranzani 1, 40127 Bologna, Italy
4 ESO – European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
5 University of Toronto, Department of Astronomy, 60 St. George Street, Toronto, Ontario, Canada M5S 3H8
6 Institute of Astronomy – ETH Hoenggerberg, HPF D8, 8093 Zurich, Switzerland
7 Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria, British Colombia, Canada V9E 2E7
8 Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
9 Observatoire de Paris, LERMA, 61 avenue de l'Observatoire, 75014 Paris, France
Corresponding author: S. Foucaud, firstname.lastname@example.org
Accepted: 25 July 2003
We present a large sample of band dropout galaxies extracted from the Canada-France deep fields survey (CFDF). Our catalogue covers an effective area of ∼1700 arcmin2 divided between three large, contiguous fields separated widely on the sky. To , the survey contains 1294 Lyman-break candidates, in agreement with previous measurements by other authors, after appropriate incompleteness corrections have been applied to our data. Based on comparisons with spectroscopic observations and simulations, we estimate that our sample of Lyman-break galaxies is contaminated by stars and interlopers (lower-redshift galaxies) at no more than . We find that is well fitted by a power-law of fixed slope, , even at small () angular separations. In two of our three fields, we are able to fit simultaneously for both the slope and amplitude and find and Mpc, and and Mpc (all spatially dependent quantities are quoted for a Λ-flat cosmology). Our data marginally indicates in one field (at a level) that the Lyman-break correlation length r0 depends on sample limiting magnitude: brighter Lyman-break galaxies are more clustered than fainter ones. For the entire CFDF sample, assuming a fixed slope we find Mpc. Using these clustering measurements and prediction for the dark matter density field computed assuming cluster-normalised linear theory, we derive a linear bias of . Finally we show that the dependence of the correlation length with the surface density of Lyman-break galaxies is in good agreement with a simple picture where more luminous galaxies are hosted by more massive dark matter halos with a simple one-to-one correspondence.
Key words: cosmology: observations / galaxies: high-redshift / galaxies: evolution / cosmology: large-scale structure of universe
Based on observations obtained at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut des Sciences de l'Univers (INSU) of the Centre National de la Recherche Scientifique and the University of Hawaii, and at the Cerro Tololo Inter–American Observatory and Mayall 4-meter Telescopes, divisions of the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc. under cooperative agreement with the National Science Foundation.
© ESO, 2003
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