The Case for Ω[TINF][ITAL]M[/ITAL][/TINF] = 0.33 ± 0.035

2001/06/30 by Michael S. Turner · 67 citations
Mathematics · Physics and Astronomy · #Anisotropy #Astrophysics #Baryon #COSMIC cancer database #Cosmic microwave background #Cosmology and Gravitation Theories #Dark matter #Galaxies: Formation, Evolution, Phenomena #Mathematics #Optics #Particle physics #Physics #Scientific Research and Discoveries #Spectral density #Statistics #astro-ph #hep-ph

paper · pdf · doi:10.1086/343782

published in The Astrophysical Journal 576(2), L101-L104 (IOP Publishing) · 4 ApJ LaTeX. Submitted to Astrophys J Lett. Less provocative title, same conclusions

arxiv created 2002/07/01 · openalex publication_date 2002/09/10 · arxiv updated 2011/05/12 · openalex created_date 2022/10/03 · openalex updated_date 2026/08/06

Abstract

For decades, the determination of the mean density of matter (Ω M ) has been tied to the distribution of light. This has led to a "bias," perhaps as large as a factor of 2, in determining a key cosmological parameter. Recent measurements of the physical properties of clusters, the cosmic microwave background anisotropy, and the power spectrum of mass inhomogeneity now allow a determination of Ω M without "visual bias." The early data lead to a consistent picture of the matter and baryon densities, with Ω B = 0.039 ± 0.0075 and Ω M = 0.33 ± 0.035, respectively.

Citations

• Measurements of Ω and Λ from 42 High‐Redshift Supernovae
• The Deuterium to Hydrogen Abundance Ratio toward a Fourth QSO: HS 0105+1619
• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Big Bang Nucleosynthesis Predictions for Precision Cosmology
• Maximum Likelihood Comparison of Tully‐Fisher and Redshift Data. II. Results from an Expanded Sample
• Final Results from theHubble Space TelescopeKey Project to Measure the Hubble Constant

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