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The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type

Madgwick, Darren S. and Hawkins, Ed and Lahav, Ofer and Maddox, Steve and Norberg, Peder and Peacock, John A. and Baldry, Ivan K. and Baugh, Carlton M. and Bland-Hawthorn, Joss and Bridges, Terry and Cannon, Russell and Cole, Shaun and Colless, Matthew and Collins, Chris and Couch, Warrick and Dalton, Gavin and De Propris, Roberto and Driver, Simon P. and Efstathiou, George and Ellis, Richard S. and Frenk, Carlos S. and Glazebrook, Karl and Jackson, Carole and Lewis, Ian and Lumsden, Stuart and Peterson, Bruce A. and Sutherland, Will and Taylor, Keith (2003) The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type. Monthly Notices of the Royal Astronomical Society, 344 (3). pp. 847-856. ISSN 0035-8711. doi:10.1046/j.1365-8711.2003.06861.x.

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We have calculated the two-point correlation functions in redshift space, ξ(σ, π), for galaxies of different spectral types in the 2dF Galaxy Redshift Survey. Using these correlation functions, we are able to estimate values of the linear redshift-space distortion parameter, β≡Ω⁰.⁶Ω/b, the pairwise velocity dispersion, a, and the real-space correlation function, ξ(r), for galaxies with both relatively low star formation rates (for which the present rate of star formation is less than 10 per cent of its past averaged value) and galaxies with higher current star formation activity. At small separations, the real-space clustering of passive galaxies is very much stronger than that of the more actively star-forming galaxies; the correlation-function slopes are, respectively, 1.93 and 1.50, and the relative bias between the two classes is a declining function of scale. On scales larger than 10 h⁻¹ Mpc, there is evidence that the relative bias tends to a constant, b_(passive)/b_(active) ≃ 1. This result is consistent with the similar degrees of redshift-space distortions seen in the correlation functions of the two classes – the contours of ξ(σ, π) require β_(active) = 0.49 ± 0.13 and β_(passive) = 0.48 ± 0.14. The pairwise velocity dispersion is highly correlated with β. Despite this, a significant difference is seen between the two classes. Over the range 8–20 h⁻¹ Mpc, the pairwise velocity dispersion has mean values of 416 ± 76 and 612 ± 92 km s⁻¹ for the active and passive galaxy samples, respectively. This is consistent with the expectation from morphological segregation, in which passively evolving galaxies preferentially inhabit the cores of high-mass virialized regions.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Norberg, Peder0000-0002-5875-0440
Baugh, Carlton M.0000-0002-9935-9755
Bland-Hawthorn, Joss0000-0001-7516-4016
Colless, Matthew0000-0001-9552-8075
Ellis, Richard S.0000-0001-7782-7071
Additional Information:© 2003 RAS. Accepted 2003 June 2. Received 2003 May 28; in original form 2003 March 31. DSM was supported by an Isaac Newton Studentship from the Institute of Astronomy and Trinity College, Cambridge. The 2dF Galaxy Redshift Survey was made possible through the dedicated efforts of the staff at the Anglo-Australian Observatory, both in creating the two-degree field instrument and supporting it on the telescope.
Funding AgencyGrant Number
University of CambridgeUNSPECIFIED
Trinity CollegeUNSPECIFIED
Subject Keywords:surveys, galaxies: distances and redshifts, galaxies: statistics, cosmological parameters, large-scale structure of Universe
Issue or Number:3
Record Number:CaltechAUTHORS:20200629-094519564
Persistent URL:
Official Citation:Darren S. Madgwick, Ed Hawkins, Ofer Lahav, Steve Maddox, Peder Norberg, John A. Peacock, Ivan K. Baldry, 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, Ian Lewis, Stuart Lumsden, Bruce A. Peterson, Will Sutherland, Keith Taylor, The 2dFGRS Team, The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type, Monthly Notices of the Royal Astronomical Society, Volume 344, Issue 3, September 2003, Pages 847–856,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104123
Deposited By: Rebecca Minjarez
Deposited On:07 Jul 2020 23:11
Last Modified:16 Nov 2021 18:28

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