Open AccessThe correlation function of X‐ray galaxy clusters in the ROSAT All‐Sky Survey 1 Bright Sample
Author(s) -
Moscardini L.,
Matarrese S.,
De Grandi S.,
Lucchin F.
Publication year - 2000
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 - 10.1046/j.1365-8711.2000.03372.x
Subject(s) - physics , rosat , astrophysics , redshift , galaxy , correlation function (quantum field theory) , cluster (spacecraft) , cluster analysis , dark matter , luminosity , galaxy cluster , cosmological constant , sky , redshift survey , luminosity function , flux (metallurgy) , dark energy , cosmology , theoretical physics , statistics , quantum mechanics , dielectric , materials science , mathematics , computer science , metallurgy , programming language
We analyse the spatial clustering properties of the ROSAT All‐Sky Survey (RASS) 1 Bright Sample, an X‐ray flux‐limited catalogue of galaxy clusters selected from the southern part of the survey. The two‐point correlation function ξ ( r ) of the whole sample is well fitted (in an Einstein–de Sitter model) by the power law ξ =( r r 0 ) − γ , with and (95.4 per cent confidence level with one fitting parameter). We use the RASS 1 Bright Sample as a first application of a theoretical model that aims to predict the clustering properties of X‐ray clusters in flux‐limited surveys for different cosmological scenarios. The model uses the theoretical and empirical relations between mass, temperature and X‐ray cluster luminosity, and fully accounts for the redshift evolution of the underlying dark matter clustering and cluster bias factor. The comparison between observational results and theoretical predictions shows that the Einstein–de Sitter models display too low a correlation length, while models with a matter density parameter Ω 0m =0.3 (with or without a cosmological constant) are successful in reproducing the observed clustering. The dependence of the correlation length r 0 on the X‐ray limiting flux and luminosity of the sample is generally consistent with the predictions of all our models. Quantitative agreement is however only reached for Ω 0m =0.3 models. The model presented here can be reliably applied to future deeper X‐ray cluster surveys: the study of the clustering properties will provide a useful complementary tool to the traditional cluster abundance analyses used to constrain the cosmological parameters.