Kinematic structure of the stellar haloes. Top three rows: Stellar density distributions in the V_R − V_ϕ plane at redshift zero for stars in the range (1 − 3)R_d (where R_d is the disc scale-length from Libeskind et al. 2020) and |z|> 1 kpc including all stars (first row), only in situ stars (second row), and only accreted populations (third row). The mass fractions of the in situ and accreted populations are shown at the bottom of the second and third rows, respectively. Bottom five rows: As above, but for the five most significant mergers at z = 0 (M1–M5; see Fig. 4 in Paper I). The merger accretion lookback time (Gyr), the 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 at the bottom of each panel. The colour bar represents a normalized density relative to the maximum value. All M31/MW HESTIA galaxies demonstrate the presence of Gaia-Sausage-like features, which exhibit different individual shapes and radial velocity ranges.