Similar to Fig. 3, but for three dwarf galaxies with stellar mass ∼10⁸ M_⋆. These examples were specifically chosen to illustrate the diversity in the colour profiles of this galaxy population and the criteria we use to we locate the edge in these different cases. In case A, we use the change in slope in the Σ_⋆ profile. In B and C, the edge is identified as a sudden transition to bluer colours in the g − r profile (see Sect. 5.4 for details). The edges of these galaxies occur at mass densities Σ_⋆(R_edge)≲2 M_⊙ pc⁻².