We report the discovery of a prominent nonthermal X-ray feature located near the Galactic center that we identify as an energetic pulsar wind nebula .
This feature , G359.95-0.04 , lies 1 lyr north of Sgr A ^ { * } ( in projection ) , is comet-like in shape , and has a power law spectrum that steepens with increasing distance from the putative pulsar .
The distinct spectral and spatial X-ray characteristics of the feature are similar to those belonging the rare class of ram-pressure confined pulsar wind nebulae .
The luminosity of the nebula at the distance of Sgr A ^ { * } , consistent with the inferred X-ray absorptions , is L _ { x } \sim 1 \times 10 ^ { 34 } { ~ { } ergs~ { } s ^ { -1 } } in the 2–10 keV energy band .
The cometary tail extends back to a region centered at the massive stellar complex IRS 13 and surrounded by enhanced diffuse X-ray emission , which may represent an associated supernova remnant .
Furthermore , the inverse Compton scattering of the strong ambient radiation by the nebula consistently explains the observed TeV emission from the Galactic center .
We also briefly discuss plausible connections of G359.95-0.04 to other high-energy sources in the region , such as the young stellar complex IRS 13 and SNR Sgr A East .