The Triangulum Galaxy (M33) shows a pronounced warp in its outer H I and stellar disk, with the gas layer bending and twisting at radii beyond the optical disk despite the galaxy being relatively low mass, nearly bulgeless, and lacking clear signs of recent major interactions or mergers (Rogstad et al. 1976; Corbelli & Schneider 1997). Standard ΛCDM explanations based on torques from a massive dark halo, minor interactions, or misaligned cold gas accretion can reproduce some warps, but the strength, coherence, and apparent isolation of M33’s warp make it difficult to ascribe uniquely to any one of these mechanisms without fine-tuning halo shape, satellite orbits, or accretion geometry (Corbelli & Schneider 1997; Corbelli & Salucci 2000).