2002/08/31 by S. W. Allen, R. W. Schmidt, A. C. Fabian +1 · 14 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06550.x
published as Mon.Not.Roy.Astron.Soc.342:287,2003 · Final version accepted for publication in MNRAS. Includes small modification of lensing analysis and an extra figure showing marginalized results on sigma_8 obtained using Chandra and lensing calibration subsamples
arxiv created 2003/02/20 · openalex publication_date 2003/06/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We present precise constraints on the normalization of the power spectrum of mass fluctuations in the nearby Universe, σ8, as a function of the mean local matter density, Ωm. Using the observed local X-ray luminosity function of galaxy clusters from the extended BCS and REFLEX studies, a mass–luminosity relation determined from Chandra and ROSAT X-ray data and weak gravitational lensing observations, and the mass function predicted by the Hubble Volume simulations of Evrard et al., we obtain σ8= (0.508 ± 0.019) Ω−(0.253±0.024)m, with Ωm < 0.34 at 68 per cent confidence. The degeneracy between σ8 and Ωm can be broken using Chandra measurements of the X-ray gas mass fractions in dynamically relaxed clusters. Using this information and including Gaussian priors on the mean baryon density of the Universe and the Hubble constant, we obtain σ8= 0.695 ± 0.042 and Ωm= 0.287 ± 0.036, for an assumed flat Λ-cold dark matter cosmology (marginalized 68 per cent confidence limits). Our results are in good agreement with some recent studies based on the local X-ray temperature function of clusters, the redshift evolution of the X-ray luminosity and temperature functions of clusters, early results from the Sloan Digitized Sky Survey, the most recent results from studies of cosmic shear, and combined analyses of the 2dF galaxy redshift survey and cosmic microwave background anisotropies.