Accelerated cosmological expansion without tension in the Hubble
  parameter
  The $H_0$-tension problem poses a confrontation of dark energy driving
late-time cosmological expansion measured by the Hubble parameter $H(z)$ over
an extended range of redshifts $z$. Distinct values $H_0\simeq 73$
km\,s$^{-1}$Mpc$^{-1}$ and $H_0\simeq 68$ km\,s$^{-1}$Mpc$^{-1}$ obtain from
surveys of the Local Universe and, respectively, $\Lambda$CBM analysis of the
CMB. These are representative of accelerated expansion with
$H^\prime(0)\simeq0$ by $\Lambda=\omega_0^2$ and, respectively, $H^\prime(0)>0$
in $\Lambda$CDM, where $\omega_0=\sqrt{1-q}H$ is a fundamental frequency of the
cosmological horizon in a Friedmann-Robertson-Walker universe with deceleration
parameter $q(z)=-1+(1+z)H^{-1}H^\prime(z)$. Explicit solutions
$H(z)=H_0\sqrt{1+\omega_m(6z+12z^2+12z^3+6z^4+(6/5)z^5)}$ and, respectively,
$H(z)=H_0\sqrt{1-\omega_m+\omega_m(1+z)^3}$ are here compared with recent data
on $H(z)$ over $0\lesssim z \lesssim2$. The first is found to be free of
tension with $H_0$ from local surveys, while the latter is disfavored at
$2.7\sigma$. A further confrontation obtains in galaxy dynamics by a finite
sensitivity of inertia to background cosmology in weak gravity, putting an
upper bound of $m\lesssim 10^{-30}$eV on the mass of dark matter. A $C^0$ onset
to weak gravity at the de Sitter scale of acceleration $a_{dS}=cH(z)$, where
$c$ denotes the velocity of light, can be seen in galaxy rotation curves
covering $0\lesssim z \lesssim 2$. Weak gravity in galaxy dynamics hereby
provides a proxy for cosmological evolution.
