Large-scale structure and the mean density of the Universe

Frenk, CS

Abstract

The density parameter, Ω, is the most important single number in models of large scale structure. At present, the two best methods to estimate it are (i) comparison of the peculiar velocity field predicted by maps of the galaxy distribution with the measured peculiar velocities of a sample of galaxy clusters and (ii) comparison of the universal baryon fraction predicted by Big Bang nucleosynthesis theory with the measured baryon fraction in rich galaxy clusters. Taken at face value, these two methods give contadictory results, Ω = 1 in the first case, and Ω ≤ 0.5 in the second. These results can be reconciled if, either Ω = 1 and the standard nucleosynthesis constraints are incorrect, or Ω ⋍ 0.4 and galaxies are substantially less clustered than the dark mass.

Citation

Frenk, C. (1995). Large-scale structure and the mean density of the Universe. Nuclear Physics B, 43(1-3), 333-342. https://doi.org/10.1016/0920-5632%2895%2900499-Y

• Journal Article Type: Article
• Online Publication Date: Jul 25, 2000
• Publication Date: 1995-06
• Journal: Nuclear Physics B
• Print ISSN: 0550-3213
• Electronic ISSN: 1873-1562
• Publisher: Elsevier
• Volume: 43
• Issue: 1-3
• Pages: 333-342
• DOI: https://doi.org/10.1016/0920-5632%2895%2900499-Y
• Keywords: COLD DARK-MATTER; IRAS GALAXIES; REDSHIFT SURVEY; VELOCITY; CLUSTERS
• Public URL: https://durham-repository.worktribe.com/output/1539711