extracted from a $r = 2\farcs64$ aperture centered on the pulsar position using 25 phase bins and computed the $\chi^2$ of the resultant profile. We find a highly significant signal ($> 8
\sigma$) at $P = 89.32842(5)$ ms at epoch 51563.314043 MJD (TBD) and $P = 89.32876(6)$ ms at epoch 51595.370251 MJD (TBD), completely consistent with the observed radio periods. The uncertainty was estimated according to the method of Leahy (1987). For each fold, we adoped the period derivative determined from the radio ephemeris. Our measurements of the period are consistent (within the errors) with the radio prediction.

In order to compare the pulse profiles for the two observations we used the phase-connected radio ephemeris to fold and align them. We present the sum and difference profiles in Figure 5. This phase alignment is completely consistent with one we computed empirically by cross-correlating the two profiles; this suggests that the  clock is stable to a few ms over a month. We can also derive the absolute radio to X-ray phase offset if we assume that the absolute time assignment is accurate (the calibration of this quantity has not yet been finalized). The phase of the radio peak relative to the 