Impact of $H_0$ priors on $f(T)$ late time cosmology. (arXiv:2108.03853v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Briffa_R/0/1/0/all/0/1">Rebecca Briffa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Escamilla_Rivera_C/0/1/0/all/0/1">Celia Escamilla-Rivera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Said_J/0/1/0/all/0/1">Jackson Levi Said</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pullicino_J/0/1/0/all/0/1">Jurgen Mifsud Nathan Lee Pullicino</a>

We present a detailed analysis of the impact of $H_0$ priors from recent
surveys in the literature on the late time cosmology of five $f(T)$
cosmological models using cosmic chronometers, the Pantheon data set, and
baryonic acoustic oscillation data. In this work, we use three recently
reported values of $H_0$ that have contributed to the recent $H_0$ tension
problem. We find that these priors have a strong response in these analyses in
terms of all the cosmological parameters. In general, our analyses gives much
higher values of $H_0$ when considered against equivalent analyses without
priors while, by and large, giving lower values of the matter density
parameter. We close with a cross-analysis of each of our model, data set and
prior combination choices.

We present a detailed analysis of the impact of $H_0$ priors from recent
surveys in the literature on the late time cosmology of five $f(T)$
cosmological models using cosmic chronometers, the Pantheon data set, and
baryonic acoustic oscillation data. In this work, we use three recently
reported values of $H_0$ that have contributed to the recent $H_0$ tension
problem. We find that these priors have a strong response in these analyses in
terms of all the cosmological parameters. In general, our analyses gives much
higher values of $H_0$ when considered against equivalent analyses without
priors while, by and large, giving lower values of the matter density
parameter. We close with a cross-analysis of each of our model, data set and
prior combination choices.

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