The Sagittarius Stream, composed of stars tidally stripped from the Sagittarius dwarf spheroidal galaxy, traces a nearly polar, wrapping orbit around the Milky Way and appears dynamically linked to the observed warp, waves, and corrugations in the Galactic disk, suggesting that repeated passages of Sagittarius have significantly perturbed the disk over the last few gigayears (Ibata et al. 2001; Ruiz-Lara et al. 2020). In ΛCDM, fitting the full 3D track, precession, and bifurcation of the Sagittarius Stream while simultaneously reproducing the Milky Way’s warp and vertical waves within a triaxial, clumpy dark-matter halo has proven difficult, because halo shapes that match the stream often misalign the disk or underpredict its warp amplitude, and models that fit the warp can fail to reproduce key features of the stream (Law & Majewski 2010; Deg & Widrow 2013).