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August 16, 20260 citationsOpen Access

Does the Galactic Acceleration Scale Track H(z)? A direct comparison of the a₀–H coincidence with the first measurements of RAR evolution

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DVDavid Rømer Voigt

Key Points

  • To test whether the galactic acceleration scale tracks the cosmic expansion rate across cosmic time and evaluate its theoretical normalization against radial acceleration relation measurements.
  • Confronted theoretical scaling predictions, where the acceleration scale evolves proportionally to the expansion rate in a Lambda-CDM model, with radial acceleration relation measurements from 79 star-forming galaxies across redshifts 0.33 < z < 1.44.
  • Separated the evaluation into two distinct tests: the functional shape of the acceleration evolution with redshift and its strict theoretical normalization scale.
  • Assessed the sensitivity of the results to systematic uncertainties in baryonic mass recalibration.
  • A constant acceleration scale across redshift is disfavored under the published calibration and modeling framework.
  • The redshift evolution of the acceleration scale remains consistent with the predicted cosmic expansion history, though decisive discrimination requires further testing.
  • The strict normalization scale is disfavored under published calibrations—implying an unphysically high local expansion rate—unless a uniform baryonic-mass offset of approximately 0.13 dex is applied.

Abstract

The galactic acceleration scale a₀ ≈ 1. 2 × 10⁻¹⁰ m s⁻² numerically satisfies a₀ ≈ cH₀/2π to within ~10%, a coincidence noted since Milgrom (1983) and still unexplained. Milgrom has long drawn the consequence: if the link is to the expansion rate rather than to Λ alone, a₀ is not constant but decreases with cosmic time, and in the deep-MOND regime rotation velocities scale as a₀^ (1/4). For a ΛCDM expansion history this fixes a specific curve, a₀ (z) ∝ H (z), rising by 76% at z = 1 and by a factor 3 at z = 2. Until recently that curve was untested at the required precision. It is no longer. Ciocan et al. (2026) have measured the radial-acceleration-relation bend scale for 79 star-forming galaxies over 0. 33 < z < 1. 44 and find a₀ increasing with redshift at high significance. This note confronts the hypothesis with that measurement, and separates two questions that must not be conflated: whether a₀ (z) follows the shape of H (z), and whether its normalisation is c/2π. The measured evolution disfavours a constant a₀ under the published modelling and calibration, and a uniform baryonic-mass recalibration cannot by itself account for the reported redshift trend; both non-evolving interpretations are therefore disfavoured under those assumptions. The tracks-H shape is not visibly ruled out by the binned estimates, but it has not been decisively tested against them, and the note states what such a test requires. The strict normalisation A = cH₀/2π is disfavoured under the published calibration, which implies H₀ ≈ 95 km s⁻¹ Mpc⁻¹; it is not excluded, since on deep-MOND scaling a uniform baryonic-mass offset of roughly 0. 13 dex — smaller than the molecular-gas systematic alone — would restore it. No mechanism is proposed, and no part of the scaling is new: the hypothesis, its adiabatic justification and the a₀^ (1/4) response are Milgrom's. What this note contributes is the confrontation itself — the separation of the two claims, the amplitude they jointly require, and an argument for why the two verdicts have different robustness against the calibration that dominates the measurement.

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Cite This Study

David Rømer Voigt (2026) studied this question.

synapsesocial.com/papers/6a817a91f2fb91fc834ae773https://doi.org/10.5281/zenodo.21950568
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