Photometrical and kinematical features imprinted by the formed ICs in the global stellar maps of the final remnants of models M6Ps[D/R]b and M6PlDb (models a to c in Table 3). Left panels: ellipticity and PA isophotal profiles of all the stars in the remnants, using an inclined view (θ = 60°, φ = 20°). The extent of the ICs as defined in Sect. 3.2.1 is indicated by vertical dashed lines in each case for reference (accordingly to Fig. 2). Right panels: 2D-maps of the kinemetric moments of the LOSVD of all the stars in the remnant using an edge-on view (V_LOS, σ, h₃, h₄). The levels are distributed linearly (simulation units). The photometric axes defined by the material in the core region of the galaxy are also plotted (straight lines). The isophotes of the stellar material in the remnant originally belonging to the satellite are overplotted for reference (contours).

Photometrical and kinematical features produced by the ICs formed, in the global stellar maps of the final remnants of models M6PlRb and M6Ps[D/R]s (models d to f in Table 3). See caption of Fig. 12.

Photometrical and kinematical features produced by the ICs formed, in the global stellar maps of the final remnants of models M9Ps[D/R]b and M18PsDb (models g to i in Table 3). See caption of Fig. 12.

Photometrical and kinematical features produced by the ICs formed, in the global stellar maps of the final remnants of models M18PsRb and M18Pl[D/R]b (models j to l in Table 3). See caption of Fig. 12.

Comparison of some ICs obtained in our minor merger experiments (first and third columns in the figure) to real observational examples with similar morphologies (second and fourth columns, respectively). The surface density maps of the ICs generated in our models are taken from Figs. 4, 5 and are in simulation units (consult captions there). The observational examples are taken from the sample of spiral galaxies with ICs developed by Erwin & Sparke (2003). Coloured maps of real galaxies correspond to B − R or V − I colour maps of these galaxies, while their grey-scale maps represent unsharp masks in V, R or H bands (see Erwin & Sparke 2003 for a detailed description of each frame). The global inclination of galaxy in the observational cases and the spatial scale of each postage stamp are indicated in each frame. In images of real galaxies, north is up and east is left, except in NGC 4665, which has been rotated 90° clockwise to emphasize the similarity with the IC resulting in experiment M6PsRb (model b). For a comparison of the scaled sizes of the ICs resulting in our models with those exhibited by real ICs, consult Sect. 4. Material from Erwin & Sparke (2003) in this figure is reproduced by permission of the American Astronomical Society (AAS) and of the original authors.