This technical preprint presents Paper II of the Holographic Residual Dark Matter framework. Paper I introduced the core CDM-like effective component. The present note focuses on the galaxy-scale phenomenology of the residual gravitational response X. In the model, the galaxy-scale residual acceleration is taken to have the MOND-like form aX = sqrt (ab aH), where ab is the baryonic Newtonian acceleration and aH is a holographic residual acceleration scale of order c H₀ / 2 pi. For an isolated galaxy with approximately fixed enclosed baryonic mass Mb at large radius, this gives aX proportional to 1/r and directly yields vf⁴ = G Mb aH, corresponding to the baryonic Tully-Fisher relation. The same scaling naturally permits extended flat circular velocities at large radii, with the eventual cutoff controlled by environment, external-field effects, boundary-memory effects, or projection-scale limitations rather than a sharp particle-halo edge. The work is presented as a phenomenological galaxy-scale consequence of the HRDM framework. It does not claim a full microscopic derivation of the residual acceleration law; rather, it identifies the mathematical consequences and observational tests of the proposed galaxy-scale response. Merging-cluster lensing/gas offsets are reserved for a subsequent note.
Ming-Ko Chung (Mon,) studied this question.