Energy-angular momentum space. Top three rows: Energy-angular momentum relation for all stars (first row), in situ stars (main progenitor, second row), and accreted stars (third row) at z = 0. To focus on the stellar halo, only stars with |z|> 1 kpc (away from the disc mid-plane) were selected. The corresponding stellar mass is shown in the bottom right of each panel. Bottom five rows: L_z − E relation for the five most significant mergers at z = 0 (M1,...,M5; see Fig. 4 in Paper I). The merger accretion lookback time (Gyr), total stellar mass of the merger debris at the time of the merger (log₁₀(M_*/M_⊙)), and the stellar mass ratio (μ_*) relative to the main M31/MW progenitor at the time of the merger are given in the bottom left corner of each panel with individual mergers debris. All colour bars represent stellar density, in units of M_⊙. The in situ stars, being kicked out from the plane, show some net rotation with some overdensities and features similar to those of the accreted stars. The latter contain a number of overdensities, which are the relics of the different merger events. Some individual merger remnants are represented by a number of features and overdensities.