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 1 + ω m (6z + 12z 2 + 12z 3 + 6z 4 + (6/5)z 5 )/(1 + z) with baryonic matter content ω 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 kpc M 1/2 11 (H 0 /H) 1 2 in galaxies of mass M = 10 11 M ⊙ 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 = ω 0 /2π, where ω 0 = √ 1 − qH is a fundamental eigenfrequency of the cosmological horizon. Extending an earlier confrontation with data covering 0.003 a N /a dS 1 at redshift z ∼ 0 in Lellie et al. (2016), the modest anomalous behavior in the Genzel et al. sample at redshifts 0.854 ≤ z ≤ 2.282 is found to be mostly due to clustering 0.36 a N /a dS 1 close to the C 0 onset to weak gravity and an increase of up to 65% in a 0 .