Similar to Fig. 10, but in (R, v_ϕ) space for the G3RV2 stars cross-matched with Galah (left), AstroNN (centre), and LAMOST (right). Density distribution (first row), colour-coded by the mean [Fe/H] (second row), the mean [Fe/H] for thin-disk stars (low-α sequence, third row), and the residual [Fe/H] distribution for low-α stars (bottom row). The coloured diagonal lines are the same as in Fig. 8 and depict the angular momentum selections in a given azimuthal range used in (X_g,Y_g) coordinates to identify overdensities in Khoperskov et al. (2020a) (see also Fig. 5). The (R, v_ϕ) density ridges are well-established structures with the higher mean metallicity (δ[Fe/H] ≈ 0.05 dex). The impact of the OLR is seen as a sharp decrease in metallicity beyond the black line.