The 2dF Galaxy Redshift Survey: luminosity dependence of galaxy clustering

被引:379
作者
Norberg, P
Baugh, CM
Hawkins, E
Maddox, S
Peacock, JA
Cole, S
Frenk, CS
Bland-Hawthorn, J
Bridges, T
Cannon, R
Colless, M
Collins, C
Couch, W
Dalton, G
De Propris, R
Driver, SP
Efstathiou, G
Ellis, RS
Glazebrook, K
Jackson, C
Lahav, O
Lewis, I
Lumsden, S
Madgwick, D
Peterson, BA
Sutherland, W
Taylor, K
机构
[1] Univ Durham, Dept Phys, Durham DH1 3LE, England
[2] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England
[3] Univ Edinburgh, Royal Observ, Astron Inst, Edinburgh EH9 3HJ, Midlothian, Scotland
[4] Anglo Australian Observ, Epping, NSW 2121, Australia
[5] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia
[6] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead L14 1LD, Merseyside, England
[7] Univ New S Wales, Dept Astrophys, Sydney, NSW 2052, Australia
[8] Univ Oxford, Dept Phys, Oxford OX1 3RH, England
[9] Univ St Andrews, Sch Phys & Astron, St Andrews KY6 9SS, Fife, Scotland
[10] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
[11] CALTECH, Dept Astron, Pasadena, CA 91125 USA
[12] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
[13] Univ Leeds, Dept Phys, Leeds LS2 9JT, W Yorkshire, England
关键词
methods : numerical; methods : statistical; galaxies : clusters : general; galaxies : formation; large-scale structure of Universe;
D O I
10.1046/j.1365-8711.2001.04839.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the dependence of the strength of galaxy clustering on intrinsic luminosity using the Anglo-Australian two degree field galaxy redshift survey (2dFGRS). The 2dFGRS is over an order of magnitude larger than previous redshift surveys used to address this issue. We measure the projected two-point correlation function of galaxies in a series of volume-limited samples. The projected correlation function is free from any distortion of the clustering pattern induced by peculiar motions and is well described by a power law in pair separation over the range 0.1 < (r/h(-1) Mpc) < 10. The clustering of L*(M-bj - 5 log(10) h = -19.7) galaxies in real space is well-fitted by a correlation length r(0) = 4.9 +/- 0.3h(-1) Mpc and power-law slope gamma = 1.71 +/- 0.06. The clustering amplitude increases slowly with absolute magnitude for galaxies fainter than M*, but rises more strongly at higher luminosities. At low luminosities, our results agree with measurements from the Southern Sky Redshift Survey 2 by Benoist et al. However, we find a weaker dependence of clustering strength on luminosity at the highest luminosities. The correlation function amplitude increases by a factor of 4.0 between M-bj - 5 log(10) h = -18 and -22.5, and the most luminous galaxies are 3.0 times more strongly clustered than L* galaxies. The power-law slope of the correlation function shows remarkably little variation for samples spanning a factor of 20 in luminosity. Our measurements are in very good agreement with the predictions of the hierarchical galaxy formation models of Benson et al.
引用
收藏
页码:64 / 70
页数:7
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