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

Licia Verde; Alan F. Heavens; Will J. Percival; Sabino Matarrese; Carlton M. Baugh; Joss Bland-Hawthorn; Terry Bridges; Russell Cannon; Shaun Cole; Matthew Colless; Chris Collins; Warrick Couch; Gavin Dalton; Roberto De Propris; Simon P. Driver; George Efstathiou; Richard S. Ellis; Carlos S. Frenk; Karl Glazebrook; Carole Jackson; Ofer Lahav; Ian Lewis; Stuart Lumsden; Steve Maddox; Darren Madgwick; Peder Norberg; John A. Peacock; Bruce A. Peterson; Will Sutherland; Keith Taylor

doi:10.1046/j.1365-8711.2002.05620.x

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

Licia Verde^*, Alan F. Heavens, Will J. Percival, Sabino Matarrese, Carlton M. Baugh, Joss Bland-Hawthorn, Terry Bridges, Russell Cannon, Shaun Cole, Matthew Colless, Chris Collins, Warrick Couch, Gavin Dalton, Roberto De Propris, Simon P. Driver, George Efstathiou, Richard S. Ellis, Carlos S. Frenk, Karl Glazebrook, Carole JacksonOfer Lahav, Ian Lewis, Stuart Lumsden, Steve Maddox, Darren Madgwick, Peder Norberg, John A. Peacock, Bruce A. Peterson, Will Sutherland, Keith Taylor

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

519 Citations (Scopus)

Abstract

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 × 10⁶ 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: b₁ = 1.04 ± 0.11, and the quadratic (non-linear) bias is consistent with zero: b₂ = -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/b₁, to yield Ω_m = 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).

Original language	English
Pages (from-to)	432-440
Number of pages	9
Journal	Monthly Notices of the Royal Astronomical Society
Volume	335
Issue number	2
DOIs	https://doi.org/10.1046/j.1365-8711.2002.05620.x
Publication status	Published - 11 Sept 2002

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Verde, L., Heavens, A. F., Percival, W. J., Matarrese, S., Baugh, C. M., Bland-Hawthorn, J., Bridges, T., Cannon, R., Cole, S., Colless, M., Collins, C., Couch, W., Dalton, G., De Propris, R., Driver, S. P., Efstathiou, G., Ellis, R. S., Frenk, C. S., Glazebrook, K., ... Taylor, K. (2002). The 2dF Galaxy Redshift Survey: The bias of galaxies and the density of the Universe. Monthly Notices of the Royal Astronomical Society, 335(2), 432-440. https://doi.org/10.1046/j.1365-8711.2002.05620.x

@article{23b08b801c7749cfa95f47716893e26d,

title = "The 2dF Galaxy Redshift Survey: The bias of galaxies and the density of the Universe",

abstract = "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 × 106 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: b1 = 1.04 ± 0.11, and the quadratic (non-linear) bias is consistent with zero: b2 = -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 ≃ Ω0.6m/b1, 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 Ωm at the effective redshift of the survey (z = 0.17).",

keywords = "Cosmological parameters, Galaxies: clusters: general, Large-scale structure of Universe",

author = "Licia Verde and Heavens, {Alan F.} and Percival, {Will J.} and Sabino Matarrese and Baugh, {Carlton M.} and Joss Bland-Hawthorn and Terry Bridges and Russell Cannon and Shaun Cole and Matthew Colless and Chris Collins and Warrick Couch and Gavin Dalton and {De Propris}, Roberto and Driver, {Simon P.} and George Efstathiou and Ellis, {Richard S.} and Frenk, {Carlos S.} and Karl Glazebrook and Carole Jackson and Ofer Lahav and Ian Lewis and Stuart Lumsden and Steve Maddox and Darren Madgwick and Peder Norberg and Peacock, {John A.} and Peterson, {Bruce A.} and Will Sutherland and Keith Taylor",

year = "2002",

month = sep,

day = "11",

doi = "10.1046/j.1365-8711.2002.05620.x",

language = "English",

volume = "335",

pages = "432--440",

journal = "Monthly Notices of the Royal Astronomical Society",

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Verde, L, Heavens, AF, Percival, WJ, Matarrese, S, Baugh, CM, Bland-Hawthorn, J, Bridges, T, Cannon, R, Cole, S, Colless, M, Collins, C, Couch, W, Dalton, G, De Propris, R, Driver, SP, Efstathiou, G, Ellis, RS, Frenk, CS, Glazebrook, K, Jackson, C, Lahav, O, Lewis, I, Lumsden, S, Maddox, S, Madgwick, D, Norberg, P, Peacock, JA, Peterson, BA, Sutherland, W & Taylor, K 2002, 'The 2dF Galaxy Redshift Survey: The bias of galaxies and the density of the Universe', Monthly Notices of the Royal Astronomical Society, vol. 335, no. 2, pp. 432-440. https://doi.org/10.1046/j.1365-8711.2002.05620.x

TY - JOUR

T1 - The 2dF Galaxy Redshift Survey

T2 - The bias of galaxies and the density of the Universe

AU - Verde, Licia

AU - Heavens, Alan F.

AU - Percival, Will J.

AU - Matarrese, Sabino

AU - Baugh, Carlton M.

AU - Bland-Hawthorn, Joss

AU - Bridges, Terry

AU - Cannon, Russell

AU - Cole, Shaun

AU - Colless, Matthew

AU - Collins, Chris

AU - Couch, Warrick

AU - Dalton, Gavin

AU - De Propris, Roberto

AU - Driver, Simon P.

AU - Efstathiou, George

AU - Ellis, Richard S.

AU - Frenk, Carlos S.

AU - Glazebrook, Karl

AU - Jackson, Carole

AU - Lahav, Ofer

AU - Lewis, Ian

AU - Lumsden, Stuart

AU - Maddox, Steve

AU - Madgwick, Darren

AU - Norberg, Peder

AU - Peacock, John A.

AU - Peterson, Bruce A.

AU - Sutherland, Will

AU - Taylor, Keith

PY - 2002/9/11

Y1 - 2002/9/11

N2 - 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 × 106 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: b1 = 1.04 ± 0.11, and the quadratic (non-linear) bias is consistent with zero: b2 = -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 ≃ Ω0.6m/b1, 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 Ωm at the effective redshift of the survey (z = 0.17).

AB - 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 × 106 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: b1 = 1.04 ± 0.11, and the quadratic (non-linear) bias is consistent with zero: b2 = -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 ≃ Ω0.6m/b1, 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 Ωm at the effective redshift of the survey (z = 0.17).

KW - Cosmological parameters

KW - Galaxies: clusters: general

KW - Large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=0005163930&partnerID=8YFLogxK

U2 - 10.1046/j.1365-8711.2002.05620.x

DO - 10.1046/j.1365-8711.2002.05620.x

M3 - Article

SN - 0035-8711

VL - 335

SP - 432

EP - 440

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

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

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