The 2dF Galaxy Redshift Survey: The bias of galaxies and the density of the Universe

By L. Verde, Alan Heavens, Will J. Percival, S. Matarrese, C. Baugh, J. Bland-Hawthorn, T. Bridges, R. Cannon, Shaun Cole, M. Colless and 20 more. 2001

497 citations recorded by the source corpus.

We compute the bispectrum of the 2dF Galaxy Redshift Survey (2dFGRS) and use it to measure the bias parameter of the galaxies. This parameter quantifies the strength of clustering of the galaxies relative to the mass in the Universe. By analysing 80 x 10 6 triangle configurations in the wavenumber range 0.1 < k < 0.5 h Mpc - 1 (i.e. on scales roughly between 5 and 30 h - 1 Mpc) we find that the linear bias parameter is consistent with unity: b 1 = 1.04 ′ 0.11, and the quadratic (non-linear) bias is consistent with zero: b 2 = -0.054 ′ 0.08. Thus, at least on large scales, optically selected galaxies do indeed trace the underlying mass distribution. The bias parameter can be combined with the 2dFGRS measurement of the redshift distortion parameter β ≃ Ω 0 . 6 m /b 1 , to yield Ωm = 0.27 ′0.06 for the matter density of the Universe, a result that is determined entirely from this survey, independent of other data sets. Our measurement of the matter density of the Universe should be interpreted as Ω m at the effective redshift of the survey (z = 0.17).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b1bc75252a4aac0bc592ec20c2c30ced50f4ca8b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

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).”
Robust Dark Energy Constraints from Supernovae, Galaxy Clustering, and 3 yr Wilkinson Microwave Anisotropy Probe Observations (2006, methodology): “However, Hawkins et al. (2003) points out that the Verde et al. (2002) results strongly depend on the assumedpairwise peculiar velocity dispersion of 385 km s 1, whileHawkins et al. (2003) finds the pairwise peculiar velocity dispersion to be 500 km s 1.”
Cosmological Parameters from the 2003 Flight of BOOMERANG (2005, methodology): “An estimate using the 3-point function and redshift space clustering distortions for 2dFGRS gives bg = 1.04 ± 0.04 (Verde et al. 2002).”
The Cosmic Energy Inventory (2004, background): “…and from dynamics, including Ωm = 0.17±0.05 from the cluster mass function as a function of redshift (Bahcall & Bode 2003) and Ωm = 0.30±0.08 from the redshift space two-point correlation function (Hawkins et al. 2003), under the assumption that the bias parameter is b = 1 (Verde et al. 2002).”
The First Cosmic Structures and Their Effects (2004, unknown): “It has been found from the 2dF Galaxy Redshift Survey that, at least on large scales (5−30h−1 Mpc), optically selected galaxies do indeed trace the underlying mass distribution (Verde et al. 2002).”
The three‐point correlation function in cosmology (2002, unknown): “These results in Figs 12 and 13 show that measuring the 3PCF could constrain halo profile properties complementary to the measurements of the 2PCF, in analogy with determinations of the galaxy bias parameter from measurements at quasi-linear scales (Feldmann et al. 2001; Verde et al. 2002).”
The Galaxy-Mass Correlation Function Measured from Weak Lensing in the Sloan Digital Sky Survey (2003, background): “On larger scales, r > 20 h 1 Mpc, there is evidence from higher order galaxy correlations (Frieman & Gaztañaga 1999; Szapudi et al. 2002; Verde et al. 2002), from the cosmic shear weak lensing power spectrum (Hoekstra, Yee, & Gladders 2002b; Jarvis et al. 2003), and from comparison of the 2dF…”
A Map of the Universe (2003, background): “…measured the cosmic microwave background in exquisite detail (Ben- nett et al. (2003)) and combined this data with other data (Percival et al. (2001); Verde et al. (2002); Croft et al. (2002); Gnedin & Hamilton (2002); Garnavich et al. (1998); Riess et al. (2001); Freedman et al. (2001);…”