Metallicty distribution functions (MDFs) for the retrograde (top), non-rotating (middle), and prograde (bottom) stars selected in the E − L_z coordinates in Fig. 5. All accreted and in situ populations are shown by the blue and red lines, respectively, while the black lines correspond to the overall distribution. The MDFs are normalised by the total mass of stars, including both accreted and in situ populations. Prograde in situ MDFs always peak at higher [Fe/H] compared to prograde accreted ones, while the two are mostly degenerate for the retrograde and non-rotating stars.