This paper applies the MMGS v1. 19 projection-layer relaxation framework to the Milky Way extended deformation formation using Gaia DR3 structural tracers with update-history stratification. The analysis inherits without modification the MMGS deformation proxy S (fixed normalization σ₀ = 20 km s⁻¹), source-rate proxy Φ, projection-layer relaxation variable ζ, radial discriminator D (R), bootstrap uncertainty σ̂D, detection threshold Ddetect, 95, and power threshold Dₘin, power. Applied to the merged Gaia DR3 sample, the retained dataset contains 45, 892 structural tracers after quality cuts and yields four populated radial bins at R = 7. 5, 8. 0, 8. 5, and 9. 0 kpc. The best-constrained bin at R = 7. 5 kpc gives D = 0. 0637 ± 0. 0512, Ddetect, 95 = 0. 1004, and Dₘin, power = 0. 1847. All retained bins satisfy D (Rj) < Dₘin, power (Rj), establishing a bounded non-detection of strong non-quasi-steady radial departure at current resolution. The paper documents the empirical meaning of the power-floor paradox: the enlarged merged run yields a best-bin power floor approximately 6. 04× worse than the earlier restricted pilot (N⋆ = 2, 292), because the age-conditioned merged pipeline degrades slope-estimator variance, not raw row count. The Milky Way projection layer is consistent with the slaved quasi-steady branch at present radial resolution, while weaker history-retaining or directionally loaded residual structure remains unresolved rather than excluded.
J. G. Villarroel H. (Sun,) studied this question.