The 2dF Galaxy Redshift Survey: The Amplitudes of fluctuations in the 2dFGRS and the CMB, and implications for galaxy biasing

By Ofer Lahav, Sarah Bridle, Will J. Percival, J. Peacock, G. Efstathiou, C. Baugh, Joss Bland-Hawthorn, T. Bridges, R. Cannon, Shaun Cole and 19 more. 2001

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We compare the amplitudes of fluctuations probed by the 2dF Galaxy Redshift Survey (2dFGRS) and by the latest measurements of the cosmic microwave background (CMB) anisotropies. By combining the 2dFGRS and CMB data, we find the linear-theory rms mass fluctuations in 8 h (-1) Mpc spheres to be sigma (8m) =0.73+/-0.05 (after marginalization over the matter density parameter Omega(m) and three other free parameters). This normalization is lower than the COBE normalization and previous estimates from cluster abundance, but it is in agreement with some revised cluster abundance determinations. We also estimate the scale-independent bias parameter of present-epoch L (s) =1.9L * APM-selected galaxies to be b (L (s) ,z =0)=1.10+/-0.08 on comoving scales of 0.02<k <0.15 h Mpc(-1). If luminosity segregation operates on these scales, L * galaxies would be almost unbiased, b (L (*) , z =0)approximate to0.96. These results are derived by assuming a flat LambdaCDM Universe, and by marginalizing over other free parameters and fixing the spectral index n =1 and the optical depth due to reionization tau =0. We also study the best-fitting pair (Omega(m) , b ), and the robustness of the results to varying n and tau . Various modelling corrections can each change the resulting b by 5-15 per cent. The results are compared with other independent measurements from the 2dFGRS itself, and from the Sloan Digital Sky Survey (SDSS), cluster abundance and cosmic shear.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6e0dc9c809737df7fb0d87c752e1efb1f66a315f

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Citations in the corpus

Weak-Lensing Results from the 75 Square Degree Cerro Tololo Inter-American Observatory Survey (2003, unknown): “Finally, as also pointed out by VW02, our likelihood contours are roughly orthogonal to those of Lahav et al. (2002) from cosmic microwave background (CMB) and 2dF Galaxy Redshift Survey constraints (see also Melchiorri & Silk 2002 for a similar investigation).”
Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra (2002, methodology): “As discussed by Lahav et al. (2002), a figure of σ8 = 0.72 is consistent with the relatively wide range of estimates from the abundance of rich clusters, but is lower than the σ8 ≃ 0.9 for Ωm ≃ 0.3 preferred by weak lensing studies.”
The Dark Side of the Halo Occupation Distribution (2003, methodology): “This normalization is suggested by several recent measurements (e.g., Borgani et al. 2001; Pierpaoli et al. 2001; Lahav et al. 2002; Schuecker et al. 2003; Jarvis et al. 2003).”
The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey (2003, methodology): “…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. 2003; Lahav et al. 2002).”
Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters (2002, result): “Our results are also in good agreement with the independent analyses of CMB+2dF data reported by Lahav et al. (2002), Percival et al. (2002) and Melchiorri & Silk (2002), the results from CMB data and Type Ia supernovae presented by Jaffe et al. (2001), and the analysis of the IRAS Point Source…”
The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications (2005, methodology): “…is the spherically averaged Kaiser linear boost factor that corrects for linear redshift distortions of L∗ galaxies at redshift zs, and b(L∗, zs) is the bias of L∗ galaxies between the real space galaxy overdensity field and the linear mass overdensity field at redshift zs (see Lahav et al. 2002).”
The REFLEX galaxy cluster survey - VII. Omega(m) and sigma(8) from cluster abundance and large-scale clustering (2002, result): “In this context it is also interesting to note that the KL results are in very good agreement with the new constraints obtained by Lahav et al. (2002) from their simultaneous analysis of the amplitudes of the fluctuations probed by the 2dF Galaxy Redshift Survey and COBE, BOOMERANG, MAXIMA1, DASI…”
The 2dF Galaxy Redshift Survey: spherical harmonics analysis of fluctuations in the final catalogue (2004, methodology): “Additionally, combining the weak-lensing constraint with our measurement of b(L∗, 0)σ8 suggests that b(L∗, 0) ∼ 0.9 in agreement with the analyses of Lahav et al. (2002) & Verde et al. (2002).”
The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type (2003, background): “As described by Lahav et al. (2002), there is now much evidence to suggest that, whilst the matter fluctuations continue to grow at low redshifts, the fluctuations in the galaxy distribution are relatively constant between 0 < z < 0.5 (see, e.g., Shepherd 2001).”
The 6dF Galaxy Survey: Samples, observational techniques and the first data release (2004, unknown): “…2004 RAS Downloaded from https://academic.oup.com/mnras/article-abstract/355/3/747/952751 by guest on 30 July 2018 mass density (Peacock et al. 2001; Percival et al. 2001; Efstathiou et al. 2002; Lahav et al. 2002; Verde et al. 2002; Zehavi et al. 2002; Hawkins et al. 2003; Szalay et al. 2003).”
The 6dF Galaxy Survey: z \approx 0 measurement of the growth rate and sigma_8 (2012, background): “Redshift-space distortion measurements are also sensitive to the overall amplitude of the clustering pattern of matter, commonly parameterised by σ8 (Lahav et al. 2002).”
Cosmological baryonic and matter densities from 600 000 SDSS luminous red galaxies with photometric redshifts (2006, background): “…the evolution of galaxy clustering, the bias factor of a class of galaxies increases with redshift in opposition to the decreasing linear growth factor, in order to reproduce the observed approximate constancy of the small-scale clustering length (e.g. Magliocchetti et al. 2000; Lahav et al. 2002).”
The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe (2002, background): “These are in good agreement with, and orthogonal to, those of Lahav et al. (2002).”
SWIRE: The SIRTF Wide‐Area Infrared Extragalactic Survey (2001, result): “…density fields are consistant only if bias is included (Dekel 1994; Strauss & Willick 1995; Rowan-Robinson et al. 2000) while other comparisons do not require bias (Willick & Strauss 1998), and recent studies of 2dFGRS redshiftspace distortions are also consistent with no bias (Lahav et al. 2002).”