[en] 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 $\mathrm{\mu <!--\; ??\; -->}=15\pm <!--\; ??\; -->7$ mas yr⁻¹ is measured, corresponding to a corrected tangential velocity of $v_{\perp <!--\; ???\; -->,c}<<!--\; <\; -->180$ km s⁻¹ 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 $\mathrm{\mu <!--\; ??\; -->}=69\pm <!--\; ??\; -->26$ mas yr⁻¹, corresponding to $v_{\perp <!--\; ???\; -->,c}=86\pm <!--\; ??\; -->33$ km s⁻¹ for a hypothetical distance of 0.3 kpc. Notably, its vector is away from the Galactic plane, although its high Galactic latitude of $b=+{37}^{\circ <!--\; ???\; -->}$ may be more a consequence of its proximity than its velocity. We also provide updated timing solutions for each pulsar. Spanning 14.5 years, 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 $B_s=9.8\times <!--\; ??\; -->{10}^{10}$ G. Calvera has $B_s=4.4\times <!--\; ??\; -->{10}^{11}$ 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 $P-<!--\; ???\; -->\stackrel{\dot{}<!--\; ??\; -->}{P}$ diagram.