Resulting kick estimates (solid blue and red lines) for the pulsars in the sample of Verbunt et al. (2017, blue and left column) and the expanded sample of Igoshev (2020, red and right column) after applying the method described in Sect. 3 to the eccentricity estimates shown in Fig. 3. The samples - consisting of N pulsars - are divided in four age ranges (i.e. τ_c ≤ 3 Myr, τ_c ≤ 10 Myr, 10 Myr < τ_c ≤ 40 Myr, 40 Myr < τ_c ≤ 1 Gyr, and the complete sample) as shown in the different rows. We fitted log-normal distributions (solid light blue/red) to the results in each panel (listed in Table 1), and to the results corresponding to the ages analysed in the literature we also fitted Maxwellians and double-Maxwellians (dashed light blue/red and grey lines, listed in Table 2). The corresponding distributions posed by Verbunt et al. (2017) and Igoshev (2020) are also shown (dotted light blue/red and grey lines). For ages 40 Myr < τ_c ≤ 1 Gyr we excluded the results for v_kick > 600 km/s (dotted blue/red lines) in the normalisation and fits. We adopted the log-normal fit to the results for the τ_c ≤ 10 Myr Igoshev sample as the fiducial natal NS kick distribution.