  We derive the Sun's offset from the local mean Galactic plane($z_\odot$)
using the observed $z$ distribution of young pulsars. Pulsar distances are
obtained from measurements of annual parallax, HI absorption spectra or
associations where available and otherwise from the observed pulsar dispersion
and a model for the distribution of free electrons in the Galaxy. We fit the
cumulative distribution function for a ${\rm sech}^2(z)$ distribution function,
representing an isothermal self-gravitating disk, with uncertainties being
estimated using the bootstrap method. We take pulsars having characteristic age
$\tau_c<10^{6.5}$~yr and located within 4.5~kpc of the Sun, omitting those
within the local spiral arm and those significantly affected by the Galactic
warp, and solve for $z_\odot$ and the scale height, $H$, for different cutoffs
in $\tau_c$. We compute these quantities using just the independently
determined distances, and these together with DM-based distances separately
using the YMW16 and NE2001 Galactic electron density models. We find that an
age cutoff at $10^{5.75}$~yr with YMW16 DM-distances gives the best results
with a minimum uncertainty in $z_\odot$ and an asymptotically stable value for
$H$ showing that, at this age and below, the observed pulsar $z$-distribution
is dominated by the dispersion in their birth locations. From this sample of
115 pulsars, we obtain $z_\odot=13.4\pm$4.4~pc and $H=56.9\pm$6.5~pc, similar
to estimated scale heights for OB stars and open clusters. Consistent results
are obtained using the independent-only distances and using the NE2001 model
for the DM-based distances.
