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The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe

Hawkins, E.; Maddox, S.; Cole, S.; Lahav, O.; Madgwick, D.S.; Norberg, P.; Peacock, J.A.; Baldry, I.K.; Baugh, C.A.; Bland-Hawthorn, J.; Bridges, T.; Cannon, R.; Colless, M.; Collins, C.; Couch, W.; Dalton, G.; De Propris, R.; Driver, S.P.; Efstathiou, G.; Ellis, R.S.; Frenk, C.S.; Glazebrook, K.; Jackson, C.; Jones, B.; Lewis, I.; Lumsden, S.; Percival, W.; Peterson, B.A.; Sutherland, W.; Taylor, K.

The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe Thumbnail


E. Hawkins

S. Maddox

O. Lahav

D.S. Madgwick

J.A. Peacock

I.K. Baldry

J. Bland-Hawthorn

T. Bridges

R. Cannon

M. Colless

C. Collins

W. Couch

G. Dalton

R. De Propris

S.P. Driver

G. Efstathiou

R.S. Ellis

K. Glazebrook

C. Jackson

B. Jones

I. Lewis

S. Lumsden

W. Percival

B.A. Peterson

W. Sutherland

K. Taylor


We present a detailed analysis of the two-point correlation function, ξ(σ, π), from the 2dF Galaxy Redshift Survey (2dFGRS). The large size of the catalogue, which contains ∼220 000 redshifts, allows us to make high-precision measurements of various properties of the galaxy clustering pattern. The effective redshift at which our estimates are made is zs≈ 0.15, and similarly the effective luminosity, Ls≈ 1.4L*. We estimate the redshift-space correlation function, ξ(s), from which we measure the redshift-space clustering length, s0= 6.82 ± 0.28 h−1 Mpc. We also estimate the projected correlation function, Ξ(σ), and the real-space correlation function, ξ(r), which can be fit by a power law (r/r0), with r0= 5.05 ± 0.26 h−1 Mpc, γr= 1.67 ± 0.03. For r≳ 20 h−1 Mpc, ξ drops below a power law as, for instance, is expected in the popular Λ cold dark matter model. The ratio of amplitudes of the real- and redshift-space correlation functions on scales of 8–30 h−1 Mpc gives an estimate of the redshift-space distortion parameter β. The quadrupole moment of ξ(σ, π) on scales 30–40 h−1 Mpc provides another estimate of β. We also estimate the distribution function of pairwise peculiar velocities, ƒ(v), including rigorously the significant effect due to the infall velocities, and we find that the distribution is well fit by an exponential form. The accuracy of our ξ(σ, π) measurement is sufficient to constrain a model, which simultaneously fits the shape and amplitude of ξ(r) and the two redshift-space distortion effects parametrized by β and velocity dispersion, a. We find β= 0.49 ± 0.09 and a= 506 ± 52 km s−1, although the best-fitting values are strongly correlated. We measure the variation of the peculiar velocity dispersion with projected separation, a(σ), and find that the shape is consistent with models and simulations. This is the first time that β and ƒ(v) have been estimated from a self-consistent model of galaxy velocities. Using the constraints on bias from recent estimates, and taking account of redshift evolution, we conclude that β (L=L*, z= 0) = 0.47 ± 0.08, and that the present-day matter density of the Universe, Ωm≈ 0.3, consistent with other 2dFGRS estimates and independent analyses.

Journal Article Type Article
Publication Date Nov 21, 2003
Deposit Date Aug 15, 2016
Publicly Available Date Aug 15, 2016
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 346
Issue 1
Pages 78-96
Keywords surveys; galaxies : distances and redshifts; galaxies : statistics; cosmological parameters; large-scale structure of UniverseCOLD DARK-MATTER; ANGULAR-CORRELATION FUNCTION; SPATIAL CORRELATION-FUNCTION; DIGITAL SKY SURVEY; POWER SPECTRUM; IRAS GALAXIES;
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Published Journal Article (600 Kb)

Copyright Statement
This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2003 RAS Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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