Pegasus-Intellectual-Capital-Solutions/Galactic-Rotation-Curves-from-the-de-Sitter-Horizon: Galactic-Rotation-Curves-from-the-de-Sitter-Horizon

The empirical MOND acceleration constant $a_0 \approx 1.2 \times 10^{-10}$ m/s² is numerically close to $cH_0/(2\pi)$ — the acceleration associated with the Gibbons–Hawking temperature of the de Sitter horizon. We define $a_u = cH_0/(2\pi)$ and test it against 171 SPARC galaxies in a 2×2 design crossing two interpolation functions with two acceleration scales, with only stellar mass-to-light ratios free. The central result is a per-galaxy comparison within MOND's own interpolation function: replacing the calibrated constant $a_0$ with $a_u = cH_0/(2\pi)$ improves the fit for 102 of 171 galaxies (59.6%, $p < 0.01$). This win-count statistic is insensitive to the choice of error floor, $\chi^2$ summary statistic, or weighting scheme. MOND simple with $a_u$ achieves the lowest median $\chi^2/\nu$ of any configuration tested (1.41), outperforming MOND simple with $a_0$ (1.53) and MOND standard (1.52) despite having zero global free parameters. The holographic interpolation independently outperforms MOND simple within the same acceleration scale (113/171, 66.1%). Both effects are robust across all error treatments and insensitive to the Hubble tension. An unconstrained scan over the acceleration scale finds a broad minimum at $a_\mathrm{best} \approx 0.75 \times 10^{-10}$ m/s$^2$; the cosmological horizon scale $a_u$ lies within this empirically allowed region and performs better than $a_0$ in the galaxy-by-galaxy comparison ($\Delta\chi^2_\mathrm{total} = +753$ vs $+1621$ above the minimum). The prediction $a_u(z) = cH(z)/(2\pi)$ provides a falsifiable distinction from both CDM and MOND. The present analysis demonstrates empirical consistency between the horizon scale and the acceleration scale required by galaxy rotation curves, rather than a unique derivation of $a_u$ from galaxy data.