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Binary mass transfer likely plays an outsized role in the evolution of massive stars comma yet direct empirical constraints on these processes remain elusive. In particular comma stars stripped by a binary companion are among the hottest sources of ionizing radiation expected at low metallicity. Such stripped stars plausibly dominate the flux of composite stellar populations at the hardest EUV energies comma and may be required to explain the puzzling high-ionization nebular emission routinely encountered in low-metallicity star-forming galaxies. But despite substantial interest and modeling effort comma only one star unambiguously stripped by binary interaction has yet been uncovered and studied in-detail. Exploratory optical spectroscopy in the extremely metal-poor (<10% solar) dwarf galaxy Leo A has recently uncovered a peculiar FUV-bright star with extremely prominent optical He II emission embedded in a small ionized nebula. Preliminary NLTE atmosphere modeling confirms that this source is broadly consistent with an intermediate mass metal-poor He star stripped by binary mass transfer yet its fundamental properties remain uncertain without spectroscopy at the FUV wavelengths where it is brightest. Here we propose COS-G160M follow-up to confirm and characterize this unique target. These observations will enable confident measurement of the luminosity comma temperature comma and mass of this likely stripped star as well as strong constraints to be placed on its wind velocity structure and mass loss rate. The serendipitous discovery of this object represents an unexpected and extremely timely opportunity for HST to directly observe a product of binary evolution at unprecendentedly-low metallicity.