  We present observations with the Chandra X-ray Observatory of the pulsar wind
nebula (PWN) within the supernova remnant G0.9+0.1. At Chandra's high
resolution, the PWN has a clear axial symmetry; a faint X-ray point source
lying along the symmetry axis possibly corresponds to the pulsar itself. We
argue that the nebular morphology can be explained in terms of a torus of
emission in the pulsar's equatorial plane and a jet directed along the pulsar
spin axis, as is seen in the X-ray nebulae powered by other young pulsars. A
bright clump of emission within the PWN breaks the axisymmetry and may
correspond to an intermediate-latitude feature in the pulsar wind.
