Radial profiles of the accumulated mass within each radius (middle panel) and volume density (bottom panel) of the old stellar content of the dwarf in the remnants of three gS0+dS0 minor-merger experiments with different orbits, compared to the original profile of the dS0 (red solid line). The remnants present different relaxation levels according to the criteria exposed in Sect. 3.2: an ongoing merger (orbit #108, green dotted-dashed line), a non-relaxed system (#106, blue short dashed line), and a fully merged and structurally relaxed remnant (#99, black long dashed line). The arrows in the top panel indicate the radius containing 10% of the initial stellar mass of the satellite in each case (see the legend). The vertical grey dotted line indicates the disc scale-length of the dS0 (a_⋆,D). Although the accumulated mass at this radius is <10% in orbits #106 and #99, the distance between the centroids of the stellar content of each progenitor is >a_⋆,D in the remnants of #106, so it is not relaxed (bottom panel). However, it is lower in the remnant of the orbit #99, thus being structurally relaxed. In #108, neither the mass accumulated at a_⋆,D is <10% nor the distance between the centroids is <a_⋆,D, hence it is an on-going merger. This classification is consistent with their morphologies in their face-on V-band mock images (top panels).