The Angular Clustering of Galaxy Pairs
Abstract
We identify close pairs of galaxies from 278 deg^2 of Sloan Digital Sky Survey commissioning imaging data. The pairs are drawn from a sample of 330,041 galaxies with 18 < r^* < 20. We determine the angular correlation function of galaxy pairs, and find it to be stronger than the correlation function of single galaxies by a factor of 2.9 +/- 0.4. The two correlation functions have the same logarithmic slope of 0.77. We invert Limber's equation to estimate the three-dimensional correlation functions; we find clustering lengths of r_0= 4.2 +/- 0.4 h^{-1} Mpc for galaxies and 7.8 +/- 0.7 h^{-1} Mpc for galaxy pairs. These results agree well with the global richness dependence of the correlation functions of galaxy systems.
Cite
@article{arxiv.astro-ph/0111019,
title = {The Angular Clustering of Galaxy Pairs},
author = {Leopoldo Infante and Michael A. Strauss and Neta A. Bahcall and Gillian R. Knapp and Robert H. Lupton and Rita S. J. Kim and Michael S. Vogeley and J. Brinkmann and Istvan Csabai and Masataka Fukugita and Gregory Hennessy and Zeljko Ivezic and Don Q. Lamb and Brian C. Lee and Jeffrey R. Pier and D. G. York},
journal= {arXiv preprint arXiv:astro-ph/0111019},
year = {2009}
}
Comments
12 pages. ApJ, in press