detail the analysis procedures required to extract quantitative information from our HRC data, in part as a cautionary tale for other early users of this instrument. We then go on to explore the morphology of the pulsar’s synchrotron nebula (§3), the soft X-ray pulse profile and limits on changes thereto (§4), and a search for changes in the nebula following the glitch (§5). The Discussion (§6) begins by developing a model which accounts for the nebula’s geometry with respect to the pulsar, as well as its anomalously low value of $L_X / \dot E$; we then go on to derive constraints on glitch models from the temporal changes we see (and don’t see) following the glitch. The final section (§7) summarizes our conclusions and assesses the prospects for future observations.

Observations
============

In response to an IAU Circular announcing a large Vela glitch on 2000 January 16.319 (Dodson et al. 2000), we submitted a Target of Opportunity request to the  Observatory (Weisskopf, O’Dell, and van Speybroeck 1996) to observe the pulsar as soon as practical, followed by a second observation roughly one month later in order to search for changes in the pulsar’s flux, pulse profile, and/or surrounding nebula. The 