Revisiting cosmological diffusion models in Unimodular Gravity and the
  $H_0$ tension
  Within the framework of Unimodular Gravity, we consider non-gravitational
interactions between dark matter and dark energy. Particularly, we describe
such interactions in the dark sector by considering diffusion models that
couple the cold dark matter fluid with the dark energy component, where the
latter has the form of a variable cosmological "constant". For the first time,
we solve the cosmological evolution of these models from the radiation
dominated era to the present day. We show how the diffusion processes take
place by analyzing the cosmological evolution of the energy density parameters
$\Omega_{cdm}$ and $\Omega_{\Lambda}$, as well as that of the Hubble parameter.
Finally, we perform the statistical analysis, imposing constraints on the
diffusion parameters, by using data from Planck 2018, SH0ES, Pantheon, and
H0LICOW collaborations. We found that cosmological diffusion models in the
framework of Unimodular Gravity can ease the current tension in the value of
$H_0$. We also show that the very far future cosmological evolution for all
diffusion models is eternally accelerating without future singularities.
