between the point source and nebula based on ROSAT HRI observations. Seward et al. (2000) attempted to isolate the pulsar emission temporally and found somewhat lower blackbody temperatures. The RXTE observations of Gurkan et al. (2000) found a similar power law index for the nebula, but a much higher normalization; while this could indicate diffuse synchrotron X-ray emission from a larger area (given their one-degree field of view), it could also result from background modeling problems, since Vela is a weak source for RXTE.

As described above, our HRC image allows us to separate cleanly the pulsar from the nebular emission. We find count rates for the pulsar and the nebula minus the pulsar (within a radius of $50^{\prime\prime}$) completely consistent with those of Markwardt and Ögelman (1998) using the Ögelman et al. (1993) spectral parameters ($kT = 0.15$ keV; $N_H = 1 \times 10^{20}$ cm$^{-2}$), confirming these as a useful characterization of the observed flux. This leads to an unabsorbed, bolometric luminosity for the pulsar blackbody emission of $\approx 1.5 \times 10^{32} d^{2}_{250}$ erg s$^{-1}$. Note, however, that this luminosity is inconsistent with the adopted temperature ($T=1.7
\times 10^6$K) and distance (250 pc) for a uniformly radiating blackbody with 