The Canada-France deep fields survey*
I. 100 000 galaxies, 1 deg: A precise measurement of to
Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille Cedex 12, France
2 University of Toronto, Department of Astronomy, 60 St. George Street, Toronto, Ontario, Canada
3 Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria, British Colombia, Canada
4 Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
5 Observatoire de Paris, DEMIRM, 61 avenue de l'Observatoire, 75014 Paris, France
Corresponding author: H. J. McCracken, firstname.lastname@example.org
Accepted: 13 July 2001
Using the University of Hawaii's 8K mosaic camera (UH8K), we have measured the angular correlation function for 100 000 galaxies distributed over four widely separated fields totalling ~ and reaching a limiting magnitude of . This unique combination of areal coverage and depth allows us to investigate the dependence of at , , on sample median magnitude in the range . Furthermore, our rigorous control of systematic photometric and astrometric errors means that fainter than we measure on scales of several arc-minutes to an accuracy of . Our results show that decreases monotonically to . At bright magnitudes, is consistent with a power-law of slope for but at fainter magnitudes we detect a slope flattening with . At the level, our observations are still consistent with . We also find a clear dependence of on observed colour. In the magnitude ranges and we find galaxies with (the reddest bin we consider) have 's which are ~ higher than the full field population. On the basis of their similar colours and clustering properties, we tentatively identify these objects as a superset of the "extremely red objects" found through optical-infrared selection. We demonstrate that our model predictions for the redshift distribution for the faint galaxy population are in good agreement with current spectroscopic observations. Using these predictions, we find that for low-Ω cosmologies and assuming a local galaxy correlation length Mpc, in the range , the growth of galaxy clustering (parameterised by ϵ), is . However, at , our observations are consistent with . Models with cannot simultaneously match both bright and faint measurements of . We show how this result is a natural consequence of the "bias-free" nature of the "ϵ" formalism and is consistent with the field galaxy population in the range being dominated by galaxies of low intrinsic luminosity.
Key words: cosmology: large-scale structure of Universe / galaxies: statistics / catalogs / astrometry / cosmology: miscellaneous
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, 2001