Evidence for galaxy dynamics tracing background cosmology below the de Sitter scale of acceleration

Galaxy dynamics probes weak gravity at accelerations below the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H$ is the Hubble parameter. Low and high redshift galaxies hereby offer a novel probe of weak gravity in an evolving cosmology, satisfying $H(z)=H_0\sqrt{1+{\omega }_m(6z+12z^2+12z^3+6z^4+(6\mathrm{/}5)z^5)}\mathrm{/}(1+z)$ with baryonic matter content ${\omega }_m$ sans tension to $H_0$ in surveys of the Local Universe. Galaxy rotation curves show anomalous galaxy dynamics in weak gravity $a_N<a_{dS}$ across a transition radius $r_t = 4.7,\mbox{kpc},M_{11}^{1/2}(H_0/H)^\frac{1}{2}$ingalaxiesofmass$M=10^{11}M_\odot M_{11}$,where$a_N$ is the Newtonian acceleration based on baryonic matter content. We identify this behavior with a holographic origin of inertia from entanglement entropy, that introduces a $C^0$ onset across $a_N=a_{dS}$ with asymptotic behavior described by a Milgrom parameter satisfying $a_0={\omega }_0\mathrm{/}2\pi$, where ${\omega }_0=\sqrt{1-q}H$ is a fundamental eigenfrequency of the cosmological horizon. Extending an earlier confrontation with data covering $0.003\lesssim a_N\mathrm{/}{a}_{dS}\lesssim 1$ at redshift $z\sim 0$ in Lellie et al. (2016), the modest anomalous behavior in the Genzel et al. sample at redshifts $0.854\le z\le 2.282$ is found to be mostly due to clustering $0.36\lesssim a_N\mathrm{/}{a}_{dS}\lesssim 1$ close to the $C^0$ onset to weak gravity and an increase of up to 65% in $a_0$.