  PSR J1813--1749 has peculiarities that make it a very interesting object of
study. It is one of the most energetic and the most scattered pulsar known. It
is associated with HESS J1813--178, one of the brightest and most compact TeV
sources in the sky. Recently, Ho et al. used archival X-ray Chandra
observations separated by more than 10 years and determined that the total
proper motion of PSR J1813--1749 is $\sim66$~mas~yr$^{-1}$, corresponding to a
velocity of $\sim$1900 km s$^{-1}$ for a distance of 6.2 kpc. These results
would imply that this pulsar is the fastest neutron star known in the Galaxy
and, by estimating the angular separation with respect to the center of the
associated supernova remnant, has an age of only $\sim300$ years, making it one
of the youngest pulsars known. Using archival high-angular-resolution VLA
observations taken over 12 years we have estimated the radio proper motions of
PSR~J1813--1748 to be much smaller:
($\mu_{\alpha}\cdot\cos(\delta),\,\mu_\delta$)=($-5.0\pm3.7,\,-13.2\pm6.7$)~mas~yr$^{-1}$,
or a total proper motion of $14.8\pm5.9$~mas~yr$^{-1}$. The positions
referenced against quasars make our results reliable. We conclude that PSR
J1813--1749 is not a very fast moving source. Its kinematic age using the new
total proper motion is $\sim1350$~years. This age is consistent within a factor
of a few with the characteristic age of the pulsar and with the age estimated
from the broadband spectral energy distribution of HESS J1813--178, as well as
the age of the associated SNR.
