  We present estimates of initial spin periods, $P_0$, for radio pulsars
associated with supernova remnants. By using the published data on 30 objects,
we were able to derive a reliable estimate for the initial spin period,
assuming standard magneto-dipole spin-down (braking index n=3), in many cases.
Our set of estimates is still not sufficient to infer the exact shape of the
initial period distribution. However, we show that a gaussian distribution with
mean and deviation $\sim 0.1$ s is consistent with our results, while flat,
wide distributions and very narrow ones are disfavored.
