Re-evaluation of $Ω_k$ of the normalised Friedmann-Lema\^ıtre-Robertson-Walker model: Implications for Hubble constant determinations

Ahmet M. Öztaş; Michael L. Smith

doi:10.1016/j.newast.2021.101609

paper

Re-evaluation of $Ω_{k}$ of the normalised Friedmann-Lema\^ıtre-Robertson-Walker model: Implications for Hubble constant determinations

arXiv:2108.05728 · doi:10.1016/j.newast.2021.101609

Abstract

The description of spacetime is an fundamental problem of cosmology. We explain why the current assignments of spacetime geometries for $Ω_{k}$ of the Friedmann-Lema\^ıtre-Robertson-Walker (FLRW) model are probably incorrect and suggest more useful descriptions. We show that $Ω_{k}$ represents not only curvature but the influence of matter density on the extent of spacetime between massive objects. Recent analyses of supernovae type Ia (SNe Ia) and HII/GEHR data with the FLRW model present the best fits with a small value for $Ω_{m}$ and a large $Ω_{k}$ . These results are consistent with our Universe exhibiting sparse matter density and quasi-Euclidean geometry and the small $Ω_{m}$ value agrees with Big Bang nucleosynthesis calculations. We suggest the geometry of our current Universe is better described by a value for $Ω_{k} \approx$ 1 rather than 0. As an example we extend the FLRW model towards the Big Bang and discover a simple explanation of how matter creation developed into the currently geometrically flat Universe with sparse, homogeneous, isotropic matter and energy distributions. Assigning $Ω_{k} \approx 1$ to describe quasi-Euclidean spacetime geometry is also useful for estimating $H_{0}$ and should help resolve the tension surrounding current estimates by different investigators.

32 pages, 5 figures, 1 table

Re-evaluation of Ωk​ of the normalised Friedmann-Lema\^ıtre-Robertson-Walker model: Implications for Hubble constant determinations

Abstract

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Re-evaluation of $Ω_{k}$ of the normalised Friedmann-Lema\^ıtre-Robertson-Walker model: Implications for Hubble constant determinations