Is the galaxy RAR scale cH₀/6? A data-first reading of 12 X-COP cluster profiles and 13 CLASH cores

The radial acceleration relation (RAR) of disc galaxies has a single scale, a₀ = (1.20 ± 0.02 ± 0.24)·10⁻¹⁰ m s⁻², numerically close to cH₀ (Milgrom: cH₀/2π; Verlinde's emergent-gravity construction: cH₀/6). Galaxy clusters show a similar low-acceleration relation with scales about ten times higher. This record looks at three measured things and then reads them with the author's framework, Mathematical Materiality (MM). The author's method is to go from the data to the framework: readings found after seeing the data are stated as such, protocols and local registrations are kept, and the checks by a second AI assistant are documented. (1) The galaxy scale. MM's two-end reading gives cH₀/2, 2.73 times the measured a₀. Dividing by 3 gives a₀ = cH₀/6 = 1.09 (H₀ = 67.4) or 1.18 (H₀ = 73.0) ·10⁻¹⁰ m s⁻², inside the measured band; in MM the factor is read as the rule used in MM 2.44 for Ω_c/Ω_b = 3√3, counted on two directions. The count, the direction of the factor and the identification with a₀ were chosen knowing the target. Approximate coherence checks: vertical density near the Sun (63.9 vs 68 ± 4 M☉ pc⁻², against 107 with cH₀/2), the 3√3 cluster baryon fraction (unchanged), the shape of a₀ ∝ H(z) (compatible with free amplitude if the MUSE-DARK III bars are 1σ). (2) Twelve X-COP clusters. A registered test of a history dependence (one scale per cluster against concentration and central entropy) gives no indication. Afterwards, declared: the scale inferred point by point with the galaxy formula decreases with radius in all twelve clusters (median slope −0.97), and a scale A/r fits every profile better than a constant. MM reading: in clusters the distal end stays approximately fixed and the governing variable becomes G·M_bar(