Open AccessModelling the two‐point correlation function of galaxy clusters in the Sloan Digital Sky Survey
Author(s) -
Basilakos Spyros,
Plionis Manolis
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07559.x
Subject(s) - physics , astrophysics , dark energy , redshift , correlation function (quantum field theory) , cluster (spacecraft) , sky , quintessence , cold dark matter , galaxy , dark matter , redshift survey , galaxy cluster , cluster sampling , cosmology , optoelectronics , dielectric , population , demography , sociology , computer science , programming language
We study the clustering properties of the recently compiled Sloan Digital Sky Survey (SDSS) cluster catalogue using the two‐point correlation function in redshift space. We divide the total SDSS sample into two richness subsamples, roughly corresponding to Abell R ≥ 0 and Automated Plate Measuring (APM) clusters, respectively. If the two‐point correlations are modelled as a power law, ξ( r ) = ( r 0 / r ) γ , then the best‐fitting parameters for the two subsamples are r 0 = 20.7 +4.0 −3.8 h −1 Mpc with γ= 1.6 +0.4 −0.4 and r 0 = 9.7 +1.2 −1.2 with γ= 2.0 +0.7 −0.5 h −1 Mpc , respectively. Our results are consistent with the dependence of cluster richness on the cluster correlation length. Finally, comparing the SDSS cluster correlation function with predictions from three flat cosmological models (Ω m = 0.3) with dark energy (quintessence), we estimate the cluster redshift‐space distortion parameter β≃Ω 0.6 m / b 0 and the cluster bias at the present time. For the Λ cold dark matter case we find β= 0.2 +0.029 −0.016 , which is in agreement with the results based on large‐scale cluster motions.