Hubble tension and matter inhomogeneities: a theoretical perspective. (arXiv:2107.14377v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Martin_M/0/1/0/all/0/1">Marco San Martín</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubio_C/0/1/0/all/0/1">Carlos Rubio</a>
We have studied how local density perturbations could reconcile the Hubble
tension. We reproduced a local void through a perturbed FLRW metric with a
potential $Phi$ which depends on both time and space. This method allowed us
to obtain a perturbed luminosity distance, which is compared with both local
and cosmological data. We got a region of local parameters, $q_0^text{Lo}$ and
$j_0^text{Lo}$, which are in agreement with a local void of
$Omega_{m,text{void}}=-0.30pm 0.15$ explaining the differences between the
local $H_0$ and the Planck $H_0$. However, when constraining local cosmological
parameters with previous results, we found that neither $Lambda$CDM nor
$Lambda(omega)$CDM could solve the Hubble tension.
We have studied how local density perturbations could reconcile the Hubble
tension. We reproduced a local void through a perturbed FLRW metric with a
potential $Phi$ which depends on both time and space. This method allowed us
to obtain a perturbed luminosity distance, which is compared with both local
and cosmological data. We got a region of local parameters, $q_0^text{Lo}$ and
$j_0^text{Lo}$, which are in agreement with a local void of
$Omega_{m,text{void}}=-0.30pm 0.15$ explaining the differences between the
local $H_0$ and the Planck $H_0$. However, when constraining local cosmological
parameters with previous results, we found that neither $Lambda$CDM nor
$Lambda(omega)$CDM could solve the Hubble tension.
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