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arxiv: astro-ph/0103143 · v1 · pith:6A7L4IEOnew · submitted 2001-03-09 · 🌌 astro-ph

A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey

J.A. Peacock , S. Cole , P. Norberg , C.M. Baugh , J. Bland-Hawthorn , T. Bridges , R.D. Cannon , M. Colless
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C. Collins W. Couch G. Dalton K. Deeley R. De Propris S.P. Driver G. Efstathiou R.S. Ellis C.S. Frenk K. Glazebrook C. Jackson O. Lahav I. Lewis S. Lumsden S. Maddox W.J. Percival B.A. Peterson I. Price W. Sutherland K. Taylor
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classification 🌌 astro-ph
keywords galaxiesclusteringomegasurveyanisotropydensitygalaxymeasurement
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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 superclusters of galaxies in the process of formation should generate 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 galaxy redshift survey. We determine the parameter beta = Omega^{0.6}/b = 0.43 +- 0.07, where Omega is the total mass-density parameter and b is a measure of the `bias' of the luminous galaxies in the survey. Combined with the anisotropy of the cosmic microwave background, our results favour a low-density universe with Omega approximately 0.3.

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