Abstract
The CNOC cluster survey was designed to measure the cluster mass to light ratio and the luminosity density of the Universe in the same range of redshifts for the purpose of estimating the parameter Ω. We find that the clusters at z ≃ 1/3 have a mean ratio of virial mass to k-corrected Gunn r luminosity of M v /L = 288 ± 49h M⊙/L⊙, where quantities are estimated with H 0 = 100h kms-1 Mpc-1 and q 0 = 0.1. The radially resolved profiles of galaxy density and velocity dispersion support the hypothesis that the clusters are effectively in equilibrium and that the galaxies are distributed similarly to the total mass. However, the virial mass needs to be reduced by a factor of 0.70 ± 0.06, on the average, to account for background contamination, which increases the virial radius, and the oft-neglected “surface term” of the virial mass estimate. In the same photometric system the mean co-moving luminosity density has a closure mass-to-light ratio of 1017±144h M⊙/L⊙. After correcting for the virial mass overestimate and the small differential evolution of galaxy luminosities in and out of clusters, we find that Ω 0 = 0.18 ± 0.05 for those components of the mass field that fall into clusters.
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© 1997 Springer-Verlag Berlin Heidelberg
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Carlberg, R.G. et al. (1997). The CNOC Cluster Survey. In: Bergeron, J. (eds) The Early Universe with the VLT. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-49709-7_27
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DOI: https://doi.org/10.1007/978-3-540-49709-7_27
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