Matching local v_R-v_ϕ features in the SNd with large-scale stellar overdensities in the guiding space of the MW. First row: number density of stars in kinematic v_R-v_ϕ space for the G3RV2 stars selected in three regions along the galactocentric radius: R = 7.8 kpc (left), R = 8.2 kpc (centre), R = 8.55 kpc (right). Colour depicts the number of stars in log-scale. Second row: unsharp-masking maps (see Eq. (2)) for corresponding density distributions. Third row: positive part of the unsharp-masking maps (overdensities), where coloured boxes highlight different isolated kinematic overdensities. Forth row: number of stars from each v_R-v_ϕ plane selected feature as a function of their angular momentum (or guiding radius). Coloured boxes depict the angular momentum selections used in (X_g,Y_g) coordinates to identify the main spiral arms of the MW, which coincide with known star-forming regions, and the bar resonances from Khoperskov et al. (2020a). In particular, the Arcturus stream (light blue) is a low-velocity tail of the Scutum-Centaurus spiral arm; part of the Hercules stream (grey) corresponds to the bar corotation, while its top part is likely to be the Sagittarius arm (blue); the Sirius stream represents the bar OLR (black); and the Hat is likely the high-velocity tail of the Perseus arm (purple).