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Title:
A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey
Authors:
Peacock, John A.; Cole, Shaun; Norberg, Peder; Baugh, Carlton M.; Bland-Hawthorn, Joss; Bridges, Terry; Cannon, Russell D.; Colless, Matthew; Collins, Chris; Couch, Warrick; Dalton, Gavin; Deeley, Kathryn; De Propris, Roberto; Driver, Simon P.; Efstathiou, George; Ellis, Richard S.; Frenk, Carlos S.; Glazebrook, Karl; Jackson, Carole; Lahav, Ofer; Lewis, Ian; Lumsden, Stuart; Maddox, Steve; Percival, Will J.; Peterson, Bruce A.; Price, Ian; Sutherland, Will; Taylor, Keith
Affiliation:
AA(), AB(Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK), AC(Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK), AD(Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK), AE(Anglo-Australian Observatory, P.O. Box 296, Epping, New South Wales 2121, Australia), AF(Anglo-Australian Observatory, P.O. Box 296, Epping, New South Wales 2121, Australia), AG(Anglo-Australian Observatory, P.O. Box 296, Epping, New South Wales 2121, Australia), AH(Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia), AI(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Birkenhead L14 1LD, UK), AJ(Department of Astrophysics, University of New South Wales, Sydney, New South Wales 2052, Australia), AK(Department of Physics, University of Oxford, Keble Road, Oxford OX3RH, UK), AL(Department of Astrophysics, University of New South Wales, Sydney, New South Wales 2052, Australia), AM(Department of Astrophysics, University of New South Wales, Sydney, New South Wales 2052, Australia), AN(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY6 9SS, UK), AO(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AP(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AQ(Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK), AR(Department of Physics & Astronomy, Johns Hopkins University, Baltimore, Maryland 21218-2686, USA), AS(Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia), AT(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), AU(Anglo-Australian Observatory, P.O. Box 296, Epping, New South Wales 2121, Australia), AV(Department of Physics, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK), AW(School of Physics & Astronomy, University of Nottingham, Nottingham NG7 2RD, UK), AX(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK), AY(Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia), AZ(Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia), BA(Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK), BB(Anglo-Australian Observatory, P.O. Box 296, Epping, New South Wales 2121, Australia)
Publication:
Nature, Volume 410, Issue 6825, pp. 169-173 (2001). (Nature Homepage)
Publication Date:
03/2001
Origin:
NATURE
Bibliographic Code:
2001Natur.410..169P

Abstract

The large-scale structure in the distribution of galaxies is thought to arise from the gravitational instability of small fluctuations in the initial density field of the Universe. A key test of this hypothesis is that forming superclusters of galaxies should generate a systematic infall of other galaxies. This would be evident in the pattern of recessional velocities, causing an anisotropy in the inferred spatial clustering of galaxies. Here we report a precise measurement of this clustering, using the redshifts of more than 141,000 galaxies from the two-degree-field (2dF) galaxy redshift survey. We determine the parameter β = Ω0.6/<ITALIC>b</ITALIC> = 0.43 +/- 0.07, where Ω is the total mass-density parameter of the Universe and b is a measure of the `bias' of the luminous galaxies in the survey. (Bias is the difference between the clustering of visible galaxies and of the total mass, most of which is dark.) Combined with the anisotropy of the cosmic microwave background, our results favour a low-density Universe with Ω ~ 0.3.
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