Velocity distribution of MS stars ejected from a binary system at the time of the first CC. Top panel: corresponding cumulative distributions. The walkaways are one order of magnitude more numerous than the runaways. The gray, blue, and red histograms show all MS secondaries, only MS stars more massive than 7.5 M_⊙ (i.e., roughly those that might experience CC), and only MS stars more massive than 15 M_⊙ (i.e., roughly the O-type stars), respectively. The mass considered here is taken right after the CC of the primary star. The dashed lines show the distribution of walkaways and runaways that have gone through RLOF (or common envelope evolution) before being ejected. Almost all massive runaways and walkaways, and the majority of the ejected stars at large velocities, have gone through RLOF. The inset plot magnifies the runaway regime v_dis ≥ 30 km s⁻¹. See also Fig. C.2 for a wider velocity range, Fig. C.1 for a figure accounting for the remaining lifetime as walkaway or runaway star, and Fig. 12 for an example of how the velocity dispersion of a star forming region affects these distributions.