Fig. E.1
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Kinematically constrained kick distributions for the sample of Verbunt et al. (2017, blue line) and the sample of pulsars that are only in the Igoshev (2020, red line) sample (i.e. the observations of Deller et al. 2019), for τc ≤ 3 Myr. The dotted lines show the kick distributions posed by Verbunt et al. (2017) and Igoshev (2020), where we note that the former is based on pulsars with τc ≤ 10 Myr instead of τc ≤ 3 Myr.
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