2005/08/31 by Masami Ouchi, M Ouchi, T. Hamana +21 · 4 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Scientific Research and Discoveries #astro-ph
paper · pdf · doi:10.1086/499519
published as Astrophys.J. 635 (2005) L117-L120 · Accepted for publication in ApJL. 5 pages, 4 figures. The text and Figures 2-4 have been revised. There is no major change which affects to the main discussion shown in the original preprint. This paper with high resolution figures is available at http://www-int.stsci.edu/~ouchi/work/astroph/sxds_z4LBG/ouchi_highres.pdf (PDF)
arxiv created 2005/11/21 · openalex publication_date 2005/12/06 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We present an angular correlation function (ACF) of z = 4 LBGs with unprecedented statistical quality, based on measurements of 16,920 LBGs obtained in the 1 deg 2 sky of the Subaru/ XMM-Newton Deep Field. The ACF significantly departs from a power law, and shows an excess on small scales. In particular, the ACFs of LBGs with i ' < 27.5 show a clear break between the small- and large-scale regimes at an angular separation of ≃7'', whose projected length corresponds to the virial radius of dark halos with a mass of 10 11 -10 12 M ☉ , indicating multiple LBGs residing in a single dark halo. At both small (2'' < θ < 3'') and large (40'' < θ < 400'') scales, clustering amplitudes increase monotonically with luminosity for the magnitude range of i ' = 24.5-27.5; the small-scale clustering shows a stronger luminosity dependence than the large-scale clustering. The small-scale bias reaches b ≃ 10-50, and the outskirts of small-scale excess extend to a larger angular separation for brighter LBGs. The ACF and number density of LBGs can be explained by the cold dark matter model.