Face-on and edge-on V-band images of S0-like remnants exhibiting some traces of past merger activity. The FoV is 100 × 100 kpc² and μ_lim(V) = 26 mag arcsec⁻² (S/N = 5) in all cases. First and third rows of panels: V-band images of the remnants in face-on and edge-on views with no smoothing, using a logarithmic grayscale that saturates in the centre to emphasise the sky noise and the fainter structures at the outskirts. Some tidal features that can be detected in each remnant are indicated in the panels. Second and fourth rows: same images as in the rows above, but using a Gaussian smoothing with σ = 10 pixels (2.5″). We have represented some isophotes (green) to emphasise the shape of the tidal features indicated in the panels above. The location of R_lim is also marked to indicate the region at which the emission of the galaxy disc falls below S/N = 5 in the image. Tidal tails in major-merger remnants tend to be small (e.g. models gSagSbo71 and gSagSdo18). One exception is the remnant of model gSagSdo2, which also contains a tidal satellite at the end of the tail. Tidal debris and plumes are observed in many models (e.g. gS0dSao106 or gSagSdo70). We have found one collisional ring (gSbgSbo70). In general, merger relics are more frequently detected in S0 remnants of minor mergers than in those of major ones for similar time evolution periods (66% vs 24%). See the caption of Fig. 5 for more details.