Results of the visual and parametric classification (see Section 3 for details). Column (3) indicates the galaxy morphological type based on Method Vis-I: El (elliptical), Sp (spiral), disc (disc galaxy with no obvious spiral arms), HD (highly disturbed: when 2 or more components are interacting and make the classification in the previous groups difficult). Column (4): type of merger based on Method Vis-II following Rodríguez Zaurín et al. (2011) and Veilleux et al. (2002): 0 = Isolated undisturbed galaxy, 0* = Isolated disturbed galaxy, 1 = two nuclei with projected separation > 1.5 kpc, 2  = two nuclei with projected separation ≤1.5 or single nucleus with signatures of a post-coalescence phase. Column (5) specifies the nature of the peculiar features based on Method Vis-III following Ramos-Almeida et al. (2011). T: tidal tail; F: fan; B: bridge; S: shell; D: dust feature; 2N: double nucleus; A: amorphous halo; I: irregular feature; IC: interacting companion. Other features we include in this work are 2N*: two nuclei with relative distance greater than 1.5 kpc; PC: projected companion, that is, there is an object close to the target in projection with no clear physical relation; K: knot; tt: streams. A question mark ‘?’ indicates uncertain classification or identification. Column (6): classification based on the parametric method (Table 5). N/A refers to objects that could not be fitted with galfit. Column (7): type of profile according to the dominant structural component: ‘HD’ in this column is for highly disturbed objects that could not be fitted with galfit. The vast majority are highly disturbed systems. Point source: a system dominated by a spatially unresolved source; disc-dominated: a system dominated by a disc or disc-like component; bulge-dominated: a system dominated by a spheroidal component. Column (8): comparison between the visual and parametric classifications.