The Two-Point Correlation of Galaxy Groups: Probing the Clustering of Dark Matter Haloes

Details The Two-Point Correlation of Galaxy Groups: Probing the Clustering of Dark Matter Haloes The Two-Point Correlation of Galaxy Groups: Probing the Clustering of Dark Matter Haloes

2004-06-25

arxiv.org/abs/astro-ph/0406593v2

Mon.Not.Roy.Astron.Soc. 357 (2005) 608-618

Astronomy and Astrophysics

Astrophysics

12 pages, 8 figures. Accepted for publication in MNRAS. Appendix added to outline the group-finder and L_18 assignment

Scientific paper

10.1111/j.1365-2966.2005.08667.x

We analyze the 2-point correlation function (2PCF) of galaxy groups identified from the 2-degree Field Galaxy Redshift Survey with the halo based group finder recently developed by Yang et al (2004b). With this group catalogue we are able to estimate the 2PCFs for systems ranging from isolated galaxies to rich clusters of galaxies. The real-space correlation length obtained for these systems ranges from $\sim 4\mpch$ to $\sim 15\mpch$, respectively. The observed correlation amplitude (and the corresponding bias factor) as a function of group abundance is well reproduced by associating galaxy groups with dark matter haloes in the standard $\Lambda$CDM model. Redshift distortions are clearly detected in the redshift-space correlation function, the degree of which is consistent with the assumption of gravitational clustering and halo bias in the cosmic density field. In agreement with previous studies we find a strong increase of the correlation length with the mean inter-group separation. Although well determined observationally, we show that current theoretical predictions are not yet accurate enough to allow for stringent constraints on cosmological parameters. Finally, we use our results to explore the power-law nature of the 2PCF of galaxies. We split the 2PCF in 1-group and 2-group terms, equivalent to the 1-halo and 2-halo terms in halo occupation models, and show that the power-law form of the 2PCF is broken, when only including galaxies in the more massive systems.

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