Studying large-scale structure with the 2dF Galaxy Redshift Survey

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dc.creatorPeacock, J. A.
dc.creatorColless, M.
dc.creatorBaldry, I.
dc.creatorBaugh, C.
dc.creatorBland-Hawthorn, J.
dc.creatorBridges, T. J.
dc.creatorCannon, R.
dc.creatorCole, S.
dc.creatorCollins, C. A.
dc.creatorCouch, W.
dc.creatorDalton, G. B.
dc.creatorDe Propris, R.
dc.creatorDriver, S. P.
dc.creatorEfstathiou, G.
dc.creatorEllis, R. S.
dc.creatorFrenk, C. S.
dc.creatorGlazebrook, K.
dc.creatorJackson, C. A.
dc.creatorLahav, O.
dc.creatorLewis, I. J.
dc.creatorLumsden, S.
dc.creatorMaddox, S. J.
dc.creatorMadgwick, D.
dc.creatorNorberg, P.
dc.creatorPercival, W.
dc.creatorPeterson, B. A.
dc.creatorSutherland, W. J.
dc.creatorTaylor, K.
dc.date2002-04-15
dc.date2002-05-28
dc.date.accessioned2026-07-07T06:28:19Z
dc.date.available2026-07-07T06:28:19Z
dc.descriptionThe 2dF Galaxy Redshift Survey is the first to observe more than 100,000 redshifts. This allows precise measurements of many of the key statistics of galaxy clustering, in particular redshift-space distortions and the large-scale power spectrum. This paper presents the current 2dFGRS results in these areas. Redshift-space distortions are detected with a high degree of significance, confirming the detailed Kaiser distortion from large-scale infall velocities, and measuring the distortion parameter beta equiv Omega_m^{0.6}/b = 0.43 +- 0.07. The power spectrum is measured to < 10% accuracy for k > 0.02 h Mpc^{-1}, and is well fitted by a CDM model with Omega_m h = 0.20 +- 0.03 and a baryon fraction of 0.15 +- 0.07. A joint analysis with CMB data requires Omega_m = 0.29 +- 0.05, assuming scalar fluctuations, but no priors on other parameters. Two methods are used to determine the large-scale bias parameter: an internal bispectrum analysis yields b = 1.04 +- 0.11, in very good agreement with the b = 1.10 +- 0.08 obtained from a joint 2dFGRS+CMB analysis, again assuming scalar fluctuations. These figures refer to galaxies of approximate luminosity 2L^*; luminosity dependence of clustering is detected at high significance, and is well described by b/b^* = 0.85 + 0.15(L/L^*).
dc.description20 Pages. To appear in "A New Era in Cosmology" (ASP Conference Proceedings), eds T. Shanks and N. Metcalfe. Replaced with minor corrections to match revised 2dFGRS bias paper
dc.identifierhttps://arxiv.org/abs/astro-ph/0204239
dc.identifierhttp://arxiv.org/abs/astro-ph/0204239
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/97662
dc.subjectAstrophysics
dc.titleStudying large-scale structure with the 2dF Galaxy Redshift Survey
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