Anisotropy of velocities of our minor merger remnants (δ) as a function of the intrinsic ellipticity at R = R_eff,glx (ϵ_intr). Stars represent the location of our models (the original primary S0b and S0c galaxies are the filled blue and green, and their remnants are the empty blue and green stars, respectively). Left panel: comparison with the distribution of real ellipticals (purple empty and filled circles) and S0s (magenta empty and filled squares) from the SAURON and ATLAS^3D samples (Burkert et al. 2008; Cappellari et al. 2013). Middle panel: comparison with to the elliptical remnants that result in major merger simulations by Burkert et al. (2008), as a function of their mass ratios (red, orange, purple, and magenta squares for 1:1, 2:1, 3:1, and 4:1, respectively). Right panel: comparison with the ellipticals remnants that result from the 1:1 and 3:1 major merger simulations by Burkert et al. (2008), considering different gas ratios, star formation, and feedback procedures. The symbols and colors used here for the Burkert et al. (2008) models are the same as used in their Fig. 3 (except for their blue triangles, which are plotted here in orange to avoid confusion with our models). For more information, we refer to that paper. Lines: different linear fits performed to the real and simulated ellipticals (consult the legend in each panel). In the left and right panels, we have overplotted the theoretical δ – ϵ_e,intr relations expected for oblate axisymmetric systems with constant values of V/σ = 0, 0.25, 0.5, 0.75, and 1.0 (see Eqs. (11)–(13) from Binney 2005). (This figure is available in color in electronic form.)