Evolution of faint galaxy clustering
The 2-point angular correlation function of 20,000 galaxies to V 23.5 and I 22.5 *
R.A. Cabanac ** 1,
V. de Lapparent 1 and
P. Hickson 2
Received 6 March 2000 / Accepted 27 June 2000
The UH8K wide field camera of the CFHT was used to image 0.68 deg2 of sky. From these images, 20,000 galaxies were detected to completeness magnitudes and . The angular correlation function of these galaxies is well represented by the parameterization . The slope shows no significant variation over the range of magnitude. The amplitude decreases with increasing magnitude in a way that is most compatible with a CDM model () with a hierarchical clustering evolution parameter . We infer a best-fit spatial correlation length of Mpc at . The peak redshift of the survey () is estimated to be , using the blue-evolving luminosity function from the CFRS and the flat cosmology, and Mpc. We also detect a significant difference in clustering amplitude for the red and blue galaxies, quantitatively measured by correlation lengths of Mpc and Mpc respectively, at .
Key words: cosmology: large-scale structure of Universe galaxies: evolution
* Based on observations from the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii
Send offprint requests to: R.A. Cabanac (email@example.com)
This article contains no SIMBAD objects.
© European Southern Observatory (ESO) 2000
Online publication: January 29, 2001