The dwarf irregular galaxy NGC 6822 shows a marked offset and kinematic misalignment between its rotating H I gas disc and its more extended stellar spheroid and halo components: the gas forms a warped, asymmetric disc, while intermediate-age and old stars (including carbon stars and RGB stars) define an elongated spheroid whose apparent rotation axis is nearly perpendicular to that of the gas, resembling a miniature polar-ring configuration (de Blok & Walter 2000; Demers et al. 2006). In ΛCDM, reproducing simultaneously the detailed H I rotation curve, the stellar kinematics, the twisted halo morphology, and the gas–star misalignment in an apparently isolated dwarf—without invoking finely tuned merger or interaction histories and specific dark-matter halo shapes—remains difficult, so NGC 6822’s offsets are often treated as a stringent test of small-scale galaxy-formation models (Weldrake et al. 2003; Kirby et al. 2014).