the pulsar along the detector $v$-axis. Examination by the instrument team found that the standard processing had failed to screen out all events flagged as instrumental. After filtering with a beta version of [SCREEN\_HRC]{} with the mask parameter set to $32771$, a much truncated jet-like feature was still apparent. In order to isolate any detector-centric artifacts, we obtained our second observation with a roll angle offset by $36^{\circ}$ from the first. As discussed below, we were able to confirm the reality of the residual jet-like feature in the cleaned images.

Independent of any filtering, the initial images showed the pulsar to be broader than the nominal PSF. To separate the pulsar from any proximate nebular emission, we followed the same phase-resolved imaging analysis described in Gotthelf & Wang (2000) for their HRC observation of PSR 0540$-$69, the 50 ms pulsar in the LMC. This separation, however, failed completely. By plotting the arrival times of the pulsar centroid, we observed that the sky coordinates of the pulsar wandered in a sinusoidal fashion with an amplitude of $0\farcs3$ and the periodicity of the programmed telescope dither. This accounted for the pulsar’s non-point-like appearance in the time-integrated image. Discussions with the  attitude aspect 