2005/11/28 by Shirley Ho, Neta Bahcall, Neta A. Bahcall +1 · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/505255
published as Astrophys.J.647:8-12,2006 · 16 pages, 4 figures
arxiv created 2005/11/28 · openalex publication_date 2006/08/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We investigate the dependence of the ellipticities of clusters of galaxies on cosmological parameters using large-scale cosmological simulations. We determine cluster ellipticities out to redshift unity for λCDM models with different mean densities Ω m and amplitudes of mass fluctuation σ 8,0 . The mean ellipticity increases monotonically with redshift for all models. Larger values of σ 8,0 , i.e., earlier cluster formation times, produce lower ellipticities. The dependence of ellipticity on Ω m is relatively weak in the range 0.2 ≤ Ω m ≤ 0.5 for high-mass clusters. The mean ellipticity ( z ) decreases linearly with the amplitude of mass fluctuations at the cluster redshift z , nearly independent of Ω m ; on average, older clusters are more relaxed and are thus less elliptical. The distribution of ellipticities about the mean is approximated by a Gaussian, allowing a simple characterization of the evolution of ellipticity with redshift as a function of cosmological parameters. At z = 0, the mean ellipticity of high-mass clusters is approximated by ( z = 0) = 0.245 - 0.070σ 8,0 + 0.020Ω m ,0 . This relation opens up the possibility that, when compared with future observations of large cluster samples, the mean cluster ellipticity and its evolution could be used as a new, independent tool to constrain cosmological parameters, especially the amplitude of mass fluctuations, σ 8,0 .