We argue that comparison with observations of theoretical models for the velocity distribution of pulsars must be done directly with the observed quantities , i.e . parallax and the two components of proper motion . We develop a formalism to do so , and apply it to pulsars with accurate VLBI measurements . We find that a distribution with two maxwellians improves significantly on a single maxwellian . The ‘ mixed ’ model takes into account that pulsars move away from their place of birth , a narrow region around the galactic plane . The best model has 42 % of the pulsars in a maxwellian with average velocity \sigma \sqrt { 8 / \pi } = 120 km/s , and 58 % in a maxwellian with average velocity 540 km/s . About 5 % of the pulsars has a velocity at birth less than 60 km/s . For the youngest pulsars ( \tau _ { c } < 10 Myr ) , these numbers are 32 % with 130 km/s , 68 % with 520 km/s , and 3 % , with appreciable uncertainties .