Top: LOS velocity profile for stars in our model (points) at time t = 200 Myr compared to observed NC stars (dashed line) (Feldmeier et al. 2014). We show the case of no rotation (left panel) and NC rotation only (right panel). The different lines refer to all stars (circles), NC stars (squares), and SC stars (diamonds) in the region defined by ﹩| x| \lt 10﹩ pc, ﹩| y| \lt 100﹩ pc, and ﹩| z| \lt 20﹩ pc. Bottom: density map of the LOS velocity (assumed to be the y-component) for all stars assuming no rotation (left panel) or NC rotation only (right panel). The kinematical signature of the SC is evident as an overdensity tilted by 108° with respect to the NC rotation axis. The density maps are smoothed via a Gaussian kernel. Black and white contours identify the loci of regions characterized by the same LOS velocity. For the sake of visibility, the contours are limited to [−20, −10, 10, 20] km s⁻¹ (left) and [−40, −30, 30, 40] km s⁻¹ (right).