X-ray profile is indicated in Figure 5.

The $\sim 200,000$ counts, uncontaminated by nebular emission, provides us with the highest signal-to-noise X-ray pulse profile for Vela yet reported (Figure 5). Greater than 99% of the counts from the blackbody component detected by the HRC fall in the $0.1-2.4$ keV ROSAT band. We compute a pulsed fraction by integrating the counts in the light curve above the lowest point and dividing by the total counts within a radius of $r=2.64^{\prime\prime}$ and subtracting the small amount of nebular background in this extraction radius (see Table 1). Our value for the pulsed fraction is $7.1 \pm 1.1\%$; the quoted error is dominated by the Poisson uncertainty in the number of counts recorded in the bin representing the light curve minimum. This value is somewhat lower than those cited above, but has the advantage of utilizing a direct measure of the total point-source contribution with subarcsecond resolution. We measure a separation between the two peaks of the main component of $\delta\phi \sim 0.325$, consistent with a linear extrapolation of the energy-dependence of this quantity reported by Strickman et al. (1999).

The background-corrected pulsar count rates were found to be $2.012
\pm 0.006$ and $1.997 