The Carina dwarf spheroidal galaxy shows hints of internal velocity gradients and kinematic substructures, with stars in different regions exhibiting slightly different line-of-sight velocities that may trace rotation, tidal stirring, or multiple stellar components (Muñoz et al. 2006; Fabrizio et al. 2011). In ΛCDM, Carina is modeled as a dark-matter-dominated, pressure-supported system where such ordered velocity gradients and complex chemo-dynamical patterns are hard to reconcile with its low mass, proximity to the Milky Way, and apparent survival against tidal disruption, often requiring finely tuned orbits and halo shapes to reproduce the observed kinematics (Lokas 2009; Battaglia & Starkenburg 2012).