Publication details for Prof Carlos FrenkMadgwick, DS, Hawkins, E, Lahav, O, Maddox, S, Norberg, P, Peacock, JA, Baldry, IK, Baugh, CM, Hawthorn, JB, 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, Lewis, I, Lumsden, S, Peterson, BA, Sutherland, W & Taylor, K (2003). The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type. Monthly Notices of the Royal Astronomical Society 344(3): 847-856.
- Publication type: Journal Article
- ISSN/ISBN: 0035-8711, 1365-2966
- DOI: 10.1046/j.1365-8711.2003.06861.x
- Keywords: surveys; galaxies : distances and redshifts; galaxies : statistics;cosmological parameters; large-scale structure of Universe2-POINT CORRELATION-FUNCTION; DIGITAL SKY SURVEY; COSMOLOGICALCONSTANT; LUMINOSITY FUNCTION; SPACE DISTORTIONS; IRAS GALAXIES; BIA
- Further publication details on publisher web site
Author(s) from Durham
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≡Ω0.6m/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, bpassive/bactive≃ 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 βactive= 0.49 ± 0.13 and βpassive= 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.