ner_tags: B-Software O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: GASP2D photometric decomposition of the mock images of the simulated galaxies is shown in Fig. 3 for the lenticular remnant resulting from the merger experiment gS0dE0o100 seen at an inclination . We listed the more relevant best-fitting structural parameters (i.e., the effective radius , Sérsic index , and axial ratio of the bulge, the scale-length and axial ratio of the disk, and the difference between the position angles of bulge and disk ) of the mock images of the simulated lenticular remnants seen at different inclinations in Table A.1 for the giant-giant galaxy mergers, Table A.2 for the giant-dwarf galaxy mergers, and Table A.3 for the giant S0-dwarf E0 galaxy mergers with different orbital parameters. Following Méndez-Abreu et al. (2017) , we adopted and as uncertainties on the axial ratio and position angle of both bulge and disk, respectively. 4.3. Bulge intrinsic shape of the simulated lenticular remnants seen at different inclinations We made use of our statistical method to retrieve from the mock images the probability distribution of the intrinsic axial ratios and of the bulges of the simulated lenticular remnants seen at different inclinations (, and ). We excluded from the analysis the edge-on configurations () because they do not allow us to constrain and due to the unknown orientation of the triaxial bulge in the disk plane. The probability distribution of and for the bulge of the simulated lenticular remnants resulting from the merger experiment gS0dE0o100 and seen at an inclination is shown as an example in Fig. 4 . The face-on configurations of the simulated lenticular remnants ( and ) provided the same result in terms of the probability distribution of and for all the simulated bulges, as expected if no observational and theoretical bias affected the adopted statistical method. Furthermore, we confirmed that the tightest constraints for are given when galaxies are seen face on, whereas remains unconstrained for these galaxies. We also found consistent probability distributions of and for the same simulated lenticular remnant seen at intermediate inclinations (, , and ). Because of this, we were confident of having correctly recovered the bulge intrinsic shape and suggested us to set a limit on the inclination of real galaxies () to robustly apply our statistical method to their bulges (see Sect. 2 ). In general, the probability distribution of and is tighter at with respect to or . Therefore, we considered this inclination as the ideal viewing angle for future analyses of the bulge intrinsic shape in real galaxies. The probability distributions of and of the bulge of the simulated lenticular remnant resulting from the merger experiment gS0dE0o100 seen at different inclinations are shown in Fig. 5 , while the remaining galaxies are in Fig. B.1 . The values of and derived for all the simulated lenticular remnants seen at different inclinations are listed in Table 1 . We realized that the accuracy of the photometric