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The 2dF Galaxy Redshift Survey: luminosity dependence of galaxy clustering
Authors:Peder Norberg  Carlton M Baugh  Ed Hawkins  Steve Maddox  John A Peacock  Shaun Cole  Carlos S Frenk  Joss Bland-Hawthorn  Terry Bridges  Russell Cannon  Matthew Colless  Chris Collins  Warrick Couch  Gavin Dalton  Roberto De Propris  Simon P Driver  George Efstathiou  Richard S Ellis  Karl Glazebrook  Carole Jackson  Ofer Lahav  Ian Lewis  Stuart Lumsden  Darren Madgwick  Bruce A Peterson  Will Sutherland  Keith Taylor
Institution:1Department of Physics, University of Durham, South Road, Durham DH1 3LE;2School of Physics &Astronomy, University of Nottingham, Nottingham NG7 2RD;3Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ;4Anglo-Australian Observatory, PO Box 296, Epping, NSW 2121, Australia;5Research School of Astronomy &Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia;6Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD;7Department of Astrophysics, University of New South Wales, Sydney, NSW 2052, Australia;8Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH;9School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY6 9SS;10Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA;11Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA;12Department of Physics &Astronomy, Johns Hopkins University, Baltimore, MD 21218-2686, USA;13Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT
Abstract:We investigate the dependence of the strength of galaxy clustering on intrinsic luminosity using the Anglo-Australian two degree field galaxy redshift survey (2dFGRS). The 2dFGRS is over an order of magnitude larger than previous redshift surveys used to address this issue. We measure the projected two-point correlation function of galaxies in a series of volume-limited samples. The projected correlation function is free from any distortion of the clustering pattern induced by peculiar motions and is well described by a power law in pair separation over the range     . The clustering of     galaxies in real space is well-fitted by a correlation length     and power-law slope     . The clustering amplitude increases slowly with absolute magnitude for galaxies fainter than M *, but rises more strongly at higher luminosities. At low luminosities, our results agree with measurements from the Southern Sky Redshift Survey 2 by Benoist et al. However, we find a weaker dependence of clustering strength on luminosity at the highest luminosities. The correlation function amplitude increases by a factor of 4.0 between     and ?22.5, and the most luminous galaxies are 3.0 times more strongly clustered than L * galaxies. The power-law slope of the correlation function shows remarkably little variation for samples spanning a factor of 20 in luminosity. Our measurements are in very good agreement with the predictions of the hierarchical galaxy formation models of Benson et al.
Keywords:methods: numerical  methods: statistical  galaxies: clusters: general  galaxies: formation  large-scale structure of Universe
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