This work presents a phenomenological mechanism within the Space–Matter–Motion (RMB) framework in which rotational motion contributes dynamically to galactic-scale spacetime response. We show that the purely local RMB formulation, based on a vorticity-dependent correction term, is insufficient to produce asymptotically flat galactic rotation curves. This motivates a minimal nonlocal extension, formulated via a memory kernel, which captures the accumulated rotational structure of the system. Using rotation-curve data from the SPARC database, we compare baryonic Newtonian predictions with RMB-guided phenomenological fits for three representative galaxies (NGC 3198, NGC 3992, and NGC 2366). The analysis demonstrates a substantial improvement in agreement with observations, including an order-of-magnitude reduction in chi-square values. These results indicate that a rotationally induced, nonlocal spacetime response may account for the observed flattening of galactic rotation curves without invoking dark matter, at least at a phenomenological level. The present implementation is not yet derived from a fully specified fundamental kernel and should be understood as a minimal, testable extension. Future work will focus on deriving the kernel structure from the full RMB field theory and establishing predictive parameter scaling across galaxy populations. The repository includes the Python code used to compute the RMB-guided fits and chi-square values. A structured overview of the RMB framework is available at: https: //grokipedia. com/page/SpaceMatterMotionTheory
Davide Dellomonaco (Tue,) studied this question.