Kinematic ages (τ_kin) versus characteristic spin-down ages (τ_c) for the pulsars in the sample of Verbunt et al. (2017, blue) and the expansion of Igoshev (2020, red) with characteristic ages below 40 Myr. The kinematic ages were determined through the sets of pulsar trajectories, where the squares are set at the median values and the whiskers show the 68% ranges. The dotted line depicts τ_kin = τ_c and the shaded region shows a 20% error on τ_c. If the median kinematic age exceeds the characteristic age with more than 5 Myr we show it as a triangle instead of a square, because the question arises whether these pulsars affect the accuracy of resulting kick distributions.