The Spin Tensor of Dark Matter and the Hubble Parameter Tension
  Allowing for a nonvanishing spin tensor for cold dark matter
($\omega_{\mathrm{DM}}=0$) has the consequence of giving rise to an effective
$\mathrm{FLRW}$ dynamics with a small negative barotropic constant for an
effective dark matter density ($-1/3<\omega_{\mathrm{eff}}\leq0$). This turns
out to solve the Hubble parameter tension in a straightforward way.
