The 2dF Galaxy Redshift Survey: the power spectrum and the matter content of the Universe

By Will J. Percival, C. Baugh, Joss Bland-Hawthorn, T. Bridges, R. Cannon, Shaun Cole, M. Colless, C. Collins, W. Couch, G. Dalton and 17 more. 2001

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The 2dF Galaxy Redshift Survey has now measured in excess of 160 000 galaxy redshifts. This paper presents the power spectrum of the galaxy distribution, calculated using a direct Fourier transform based technique. We argue that, within the k-space region 0.02 less than or similar to k less than or similar to 0.15 h Mpc(-1), the shape of this spectrum should be close to that of the linear density perturbations convolved with the window function of the survey. This window function and its convolving effect on the power spectrum estimate are analysed in detail. By convolving model spectra, we are able to fit the power-spectrum data and provide a measure of the matter content of the Universe. Our results show that models containing baryon oscillations are mildly preferred over featureless power spectra. Analysis of the data yields 68 per cent confidence limits on the total matter density times the Hubble parameter Omega (m) h = 0.20 +/- 0.03, and the baryon fraction Omega (b)/Omega (m) = 0.15 +/- 0.07, assuming scale-invariant primordial fluctuations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6a895341bd84cc2cede5eb9fd17f7d4952dece75

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Citations in the corpus

The REFLEX galaxy cluster survey - VII. Omega(m) and sigma(8) from cluster abundance and large-scale clustering (2002, background): “…Bahcall & Fan 1998, Eke et al. 1998, Henry 2000, Borgani et al. 2001, Reiprich & Böhringer 2002, hereafter RB02), and from the large-scale distribution of clusters (e.g. Collins et al. 2000, Schuecker et al. 2001, hereafter Paper I) and galaxies (e.g., Percival et al. 2001, Szalay et al. 2001).”
The Dark Matter Distribution in the Central Regions of Galaxy Clusters: Implications for Cold Dark Matter (2003, background): “…of the universe on large scales at various epochs, from that of the cosmic microwave background, through high redshift studies of the Lyα forest to the distribution of galaxies and clusters in local surveys (e.g. Percival et al. 2001, Spergel et al. 2003; Croft et al. 2002; Bahcall et al. 2003).”
Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys (2003, background): “Recent analyses of large surveys may be beginning to reveal these features (Percival et al. 2001; Miller et al. 2001) There have been numerous studies on how the combination of CMB anisotropy data and large-scale structure data, either present (Scott, Silk, & White 1995; Gawiser & Silk 1998; Lange…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, background): “…most studies in the past evaluated equation (29) as a convolution with the spherically averaged window function, Ws (see e.g. Laix & Starkman 1997; Percival et al. 2001, 2007; Cole et al. 2005; Ross et al. 2012b): P conv(k) = ∫ d P true(k + )|W ( )|2s (30) which assumes an isotropic power…”
Toward a Precise Measurement of Matter Clustering: Lyα Forest Data at Redshifts 2-4 (2000, methodology): “Recent estimates of the galaxy power spectrum from the 2dF Galaxy Redshift Survey find best-fit parameter combinations Ωmh = 0.20 and Ωb/Ωm = 0.15 for a CDM model with scale-invariant initial fluctuations (Percival et al. 2001).”
An alternative to the cosmological 'concordance model' (2003, result): “6, both models are then in agreement with the APM power spectrum (Baugh & Efstathiou 1993; Peacock 1997), the 2dFGRS power spectrum (Percival et al. 2001; Tegmark, Hamilton & Xu 2002) and the Lyα forest (matter) power spectrum (Croft et al. 2002) which has been used recently to set interesting…”
Subaru Deep Survey. VI. A Census of Lyman Break Galaxies at z ≃ 4 and 5 in the Subaru Deep Fields: Clustering Properties (2003, methodology): “Clustering properties of galaxies are closely related to the distribution and amount of underlying dark matter (e.g., Peacock et al. 2001; Percival et al. 2001; Verde et al. 2002; Percival et al. 2002; Szalay et al. 2003).”
Observational probes of cosmic acceleration (2012, background): “Early results from the 2dF Galaxy Redshift Survey (2dFGRS) (Percival et al., 2001; Efstathiou et al., 2002; Percival et al., 2002) and the Abell/ACO cluster sample (Miller et al.”
The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey (2003, methodology): “Tantalizing evidence for baryonic wiggles in the galaxy power spectrum is presented by Percival et al. (2001) and Miller et al. (2001a,b, 2002), and cosmological models have been further constrained in conjunction with cosmic microwave background (CMB) data (e.g., Spergel et al. 2003; Verde et al.…”
Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra (2002, methodology): “Similarly, large scale structure (LSS) power spectra were calculated for the relevant models using the fitting formula of Eisenstein & Hu (1998), and were convolved with the window function of the 2dFGRS sample, before being compared to the 2dFGRS data as in Percival et al. (2001).”
Galaxy and mass assembly (GAMA): End of survey report and data release 2 (2015, methodology): “…al. 2000; Alam et al. 2015) demonstrated convincingly that the description of large-scale structure formation provided by the cold dark matter (CDM) paradigm is remarkably accurate (e.g. Peacock et al. 2001; Percival et al. 2001, 2007; Tegmark et al. 2004; Cole et al. 2005; Eisenstein et al. 2005).”
The power spectrum of SUSY-CDM on subgalactic scales (2003, background): “…with the observed abundances of light elements and primordial nucleosynthesis (see e.g. Tyler et al. 2000) and the power spectrum found from galaxy redshift surveys (Percival et al. 2001), and indicate that the Universe contains a significant amount of non-baryonic cold dark matter (CDM).”