Same as Fig. 7 but for G31. Since G31 experienced a major merger, a large fraction of CR stellar disk (i.e., ϵ_*< -0.5) is displayed in the outer parts. A clear signature of this is the higher fraction in mass of counter-rotating stars in the outer parts with respect to co-rotating stars (upper panel, red line). Other potential signatures lie in the mean age and mean mellaticity of counter-rotating stars with constant values at larger radius (here r> 4 kpc). We note that the mean metallicity of log(Z/Z_⊙)∼-0.25 is proved to match with the mean metallicity of the satellite prior the merger event.