The galactic distribution of pulsars and shell remnants of supernovae (SN) as investigated on the basis of newly-estimated parameters. Special attention was paid to taking into account all possible selection effects and an attempt was made to reveal a statistically-pure ensemble of objects. On the basis of this ensemble we studied the radial andz-distribution of pulsars and supernova remnants (SNR). It is shown that the radial distribution of both objects is considered to have an annular structure with the maximum surface density at a distance of 4.5 5.3 kpc (if the distance of the Sun from the galactic centre is assumed to be equal to 8.5 kpc). The scle-height of the progenitors of SNRs is not more than 110 pc and only 15% of the SNRs, whose progenitors may also be massive runaway stars, are situated at ∼300 pc. The mean application of the pulsars is not more than ∼300 pc which agrees with the hypothesis about the genetic connection with type-II SN outbursts at the kinematic aget k∼5×106 yr and thez-component of spatial velocity beingV z=120 km s-1. The possible precursors of type-I SNRs by the shape of their radial distribution in late spirals and the various model calculations given in the literature, are also discussed.