Top row, left panel: Gaia (U, V) kinematics in the solar neighbourhood from Fig. 8; the contours contain 50, 68, 80, 90, and 99% of the stars. Top row, right panel: as in the left panel, but here the stars are plotted in the space of actions (J_ϕ − J_circ, J_R); the actions are computed assuming the P17 background potential, the epicyclic approximation, and (U_⊙, V_⊙) = (11.1, 0) km s⁻¹; J_circ is the angular momentum of a circular orbit at the Sun. Bottom row, left panel: (u, v) distribution at the Sun obtained via backward integration from Fig. 8; the contours contain 50, 68, 80, 90, and 95% of the stars. Bottom row, right panel: as in the left panel, but here the stars are plotted in the space of actions (J_ϕ − J_circ, J_R). In all the plots the coloured lines represent the same and corresponding positions in the (u, v), (J_ϕ − J_circ, J_R), and (U, V) spaces. Shown is the effect of the CR (Hercules, green line), 6:1 (horn, purple line), and 4:1 (blue line) on both the model and data. The 2:1 resonance (red line) is also present in both, and most prominently seen in action space, but with a slight position mismatch between model and data, linked to the choice of V_⊙ and the shape of the circular velocity curve of the axisymmetric background (see text). Also shown is the prominent deformation in the velocity plane of the data at (U, V) ∼ (−35, −15) km s⁻¹, namely the Hyades moving group, which is not reproduced by our bar-only model, and which has long been suspected to be related to a spiral perturbation.