The dwarf galaxy Leo T is an extremely faint, gas-rich Local Group satellite whose neutral hydrogen and stellar components show subtle spatial and kinematic offsets, along with ongoing star formation despite global stability criteria suggesting its gas should not readily collapse (Irwin et al. 2007; Ryan-Weber et al. 2008). In ΛCDM, Leo T is modeled as a highly dark-matter–dominated system near the Milky Way’s virial radius, but simultaneously explaining its high mass-to-light ratio, retained cold gas, gentle infall orbit, and offset gas–star morphology without fine-tuned combinations of dark halo structure, feedback, and environmental stripping remains challenging, making Leo T an important small-scale test of the standard paradigm (Simon 2019; Read et al. 2024).