($r>52.7^{\prime\prime}$). We extracted counts from the pulsar using a circular aperture 264 in radius and estimated background from the surrounding annulus, $2\farcs64 < r < 3\farcs43$. Table 1 summarizes the properties of the individual components, including their estimated sizes and intensities.

[rcc]{} A) Pulsar (Obs 1)& point-like & $2.012 \pm 0.006$ (Obs 2)& & $1.997 \pm 0.007$ B) Nebula (Obs 1)& $20^{\prime\prime} \times 10^{\prime\prime}$ NE-SW & $2.720 \pm 0.007$ (Obs 2)& & $2.762 \pm 0.008$ C) Arc (Obs 1)& & $0.675 \pm 0.004$ (Obs 2)& & $0.700 \pm 0.004$ D) Jet (Obs 1)& $10^{\prime\prime}$ long SE-NW & $0.037 \pm 0.001$ (Obs 2)& & $0.036 \pm 0.001$

The best current measurements for the Vela pulsar and remnant place it at a distance of only $250\pm30$ pc (Cha, Sembach, and Danks 1999 and references therein); in all that follows we scale by $d = 250 d_{250}$ pc.

Vela X, the $\sim 100^{\prime}$ diameter, flat-spectrum radio component near the center of the Vela remnant (Milne 1968; Bock et al. 1998) is generally regarded as the pulsar’s radio synchrotron nebula. While soft X-rays from this region are detected, they are primarily thermal in nature, and represent emission from the hot plasma which fills the 