Late time transitions in the quintessence field and the $H_0$ tension. (arXiv:1906.11255v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_E/0/1/0/all/0/1">Eleonora Di Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferreira_R/0/1/0/all/0/1">Ricardo Z. Ferreira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Visinelli_L/0/1/0/all/0/1">Luca Visinelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Danielsson_U/0/1/0/all/0/1">Ulf Danielsson</a>
We consider a quintessence field which transitions from a matter-like to a
cosmological constant behavior between recombination and the present time. We
aim at easing the tension in the measurement of the present Hubble rate, and we
assess the $Lambda$CDM model properly enlarged to include our quintessence
field against cosmological observations. The model does not address the scope
we proposed. This result allows us to exclude a class of quintessential models
as a solution to the tension in the Hubble constant measurements.
We consider a quintessence field which transitions from a matter-like to a
cosmological constant behavior between recombination and the present time. We
aim at easing the tension in the measurement of the present Hubble rate, and we
assess the $Lambda$CDM model properly enlarged to include our quintessence
field against cosmological observations. The model does not address the scope
we proposed. This result allows us to exclude a class of quintessential models
as a solution to the tension in the Hubble constant measurements.
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