The dipole functions in quasispherical Szekeres models shift shells relative to each other and rotate their local frames by exact amounts, and the paper shows how these effects explain the models' geometry.
The Metric of the Cosmos from Luminosity and Age Data
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abstract
This paper presents the algorithm for determining the Lemaitre-Tolman (LT) model that best fits given datasets for maximum stellar ages, and SNIa luminosities, both as functions of redshift. It then applies it to current cosmological data. Special attention must be given to the handling of the origin, and the region of the maximum diameter distances. As with a previous combination of datasets (galaxy number counts and luminosity distances versus redshift), there are relationships that must hold at the region of the maximum diameter distance, which are unlikely to be obeyed exactly by real data. We show how to make corrections that enable a self-consistent solution to be found. We address the questions of the best way to approximate discrete data with smooth functions, and how to estimate the uncertainties of the output - the 3 free functions that determine a specific LT metric. While current data does not permit any confidence in our results, we show that the method works well, and reasonable LT models do fit with or without a cosmological constant.
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gr-qc 1years
2019 1verdicts
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Physical geometry of the quasispherical Szekeres models
The dipole functions in quasispherical Szekeres models shift shells relative to each other and rotate their local frames by exact amounts, and the paper shows how these effects explain the models' geometry.