  Through adaptive optics (AO) imaging with the SOUL+LUCI instrument at the
Large Binocular Telescope we were able to resolve, for the first time,
individual stars in the gas-rich galaxy DDO68 C. This system was already
suggested to be interacting with the extremely metal poor dwarf DDO68, but its
nature has remained elusive so far because of the presence of a bright
foreground star close to its line of sight, that hampers a detailed study of
its stellar population and distance. In our study, we turned this interloper
star into an opportunity to have a deeper insight on DDO68 C, using it as a
guide star for the AO correction. Although the new data do not allow for a
direct distance measurement through the red giant branch tip method, the
combined analysis of the resolved-star color-magnitude diagram, of archival
GALEX FUV and NUV photometry, and of H$\alpha$ data provides a self-consistent
picture in which DDO68 C is at the same $\sim$13 Mpc distance as its candidate
companion DDO68. These results indicate that DDO68 is a unique case of a low
mass dwarf, less massive than the Magellanic Clouds, interacting with three
satellites (DDO68 C and two previously confirmed accreting systems), providing
useful constraints on cosmological models and a potential explanation for its
anomalous extremely low metallicity.
