low-mass galactic merger in a cosmological context because of the differences in scales. Although limited in resolution, studies in the context of the Local Group demonstrated that a significant fraction of present-day dwarfs underwent a significant merger with another dwarf galaxy in the past [@kli10; @dea14]. These mergers most likely occur early on, at the outskirts of the Local Group and between bound pairs or within groups. @kaz11 demonstrated that mergers between initially disky dwarf galaxies may produce pressure-supported systems with parameters very similar to those of dwarf spheroidal (dSph) galaxies found in the Local Group. These systems seem particularly suitable for testing the merger paradigm on small scales as their proximity offers a possibility for high-resolution measurements.

A few candidates for merger remnants have been already identified among the dSph galaxies of the Local Group. The first was the Fornax dwarf for which shells of stars in the vicinity of the main body were observed [@col05]. Other cases may include the most distant dSphs such as Cetus and Tucana that could not have interacted with the Milky Way and M31 very strongly in the past and be tidally transformed so the merger scenario seems particularly plausible [@kaz11], though hypothetical 