observations were carried out on 20 January 2000 and 21 February 2000, $\sim 3.5$ and $\sim 35$ days after the glitch using the  imaging High Resolution Camera (HRC-I; Murray et al. 1997). Integration times of $\sim 50$ ksec were achieved in both observations.

The HRC-I detector on-board  is sensitive to X-rays over the $0.08-10.0$ keV range, although essentially no energy information on the detected photons is available. Photons are time-tagged with a nominal precision of 15.6 $\mu$s; in this work, their arrival times were corrected to the solar system barycenter using a beta version of [AXBARY]{}. The data were collected during a portion of the orbit which avoided regions of high background contamination from the bright Earth and radiation belt passages; the second observation was, however, found to be partially contaminated by particle activity, most likely of solar wind origin (see below). The pulsar was centered at the on-axis position of the HRC where the point-spread function (PSF) has a minimum half-power diameter (the radius enclosing 50% of total source counts) of $\sim 0\farcs5$, which increases with energy. Images were extracted centered on the pulsar and binned using the native HRC $0\farcs13175 \times 0\farcs13175$ pixel size into $1024 \times 1024$ 