2003/02/16 by Nelson Padilla, N. D. Padilla, D. G. Lambas · 2 citations
Medicine · Physics and Astronomy · #Anisotropy #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Cosmic Phenomena #Brightest cluster galaxy #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Galaxy groups and clusters #Medicine #Observational study #Optics #Physics #Redshift #Redshift survey #Redshift-space distortions #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06570.x
12 pages, 10 figures. Revised version re-submitted to MNRAS. Info and figures can be found at http://star-www.dur.ac.uk/~nelsonp/anisotropies
arxiv created 2003/02/16 · openalex publication_date 2003/06/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study the redshift space correlation function of galaxy clusters for observational samples constructed in different surveys. We explore correlation amplitudes, pairwise velocity distributions and bias factors. Systematics in cluster identification procedures are the main source of biased estimates of the correlation amplitude and inferred velocity dispersions. By comparing our results with those of numerical simulations we explore the strong influence on the clustering distortion pattern in redshift space from effects associated with the cluster identification procedure from two dimensional surveys as is the case of Abell and APM clusters. The identification of clusters in X-ray surveys improves this situation, although there are still systematic effects which are probably due to identification of optical sources in the determination of cluster redshifts. These systematics are particularly strong for the most luminous X-ray selected clusters in the Extended Bright Cluster Survey, which exhibits very large anisotropies, comparable to those present in the Abell catalogue. Our results demonstrate that forthcoming large redshift surveys will be extremely important for the construction of new samples of groups and clusters as well as improving the determination of optical and X-ray selected cluster distances, essential for reliable analyses of the large scale structure.