Evolution of the distribution of the perpendicular velocity V_⊥ of the surrounding gas relative to the local filament frame in the two simulations High_B (red), Low_B (blue). Looking across the columns, the distributions are shown at three different radial offsets from the filament crest (0.05 pc, 0.1 pc, 0.2 pc), while the temporal evolution is displayed across the rows at different SFE of the cloud (0.1%, 3%, 6%) and 0.3 Myr after the onset of the main H II region (last row). The black dot-dashed lines give a reference sound speed for a molecular medium at 10 K. The overall preference towards negative V_⊥ highlights how filaments never stop accreting. The widening of the wings during the feedback-dominated phase suggests more random velocities (cf. Fig. 8).