  Using pairs of images from the Chandra High-Resolution Camera we examine the
proper motion of the central compact object (CCO) 1E 1207.4-5209 in the
supernova remnant (SNR) PKS 1209-51/52, and the unusual pulsar Calvera that is
possibly a CCO descendant. For 1E 1207.4-5209, an insignificant proper motion
of 15+/-7 mas/yr is measured, corresponding to a corrected tangential velocity
of <180 km/s at the distance of 2 kpc. This proves that the previously noted
large offset of the pulsar from the apparent geometric center of the SNR is not
due to high proper motion; evidently the symmetry of the remnant does not
indicate its center of expansion. Calvera has a marginally significant proper
motion of 69+/-26 mas/yr, corresponding to 86+/-33 km/s for a hypothetical
distance of 0.3 kpc. Notably, its vector is away from the Galactic plane,
although its high Galactic latitude of b = +37 deg may be more a consequence of
its proximity than its velocity. We also provide updated timing solutions for
each pulsar. Spanning 14.5 yr, the ephemeris of 1E 1207.4-5209 has a small and
steady frequency derivative that, because of the negligible proper motion,
requires no kinematic correction. The derived surface dipole magnetic field
strength of 1E 1207.4-5209 thus remains B_s = 9.8e10 G. Calvera has B_s =
4.4e11 G, intermediate between those of ordinary young pulsars and CCOs,
suggesting that it may be on a trajectory of field growth that could account
for the absence of descendants in the neighborhood of CCOs in the P-Pdot
diagram.
