  We have examined Chandra observations of the recently discovered X-ray thread
G0.13-0.11 in the Galactic center Radio Arc region. Part of the {\sl Chandra}
data was studied by Yusef-Zadeh, Law, & Wardle (2002), who reported the
detection of 6.4-keV line emission in this region. We find, however, that this
line emission is {\sl not} associated with G0.13-0.11. The X-ray spectra of
both G0.13-0.11 and the point-like source embedded are well characterized by a
power law. The 2 -- 10 keV band luminosities of these two components are $\sim
3.2\times 10^{33}{\rm ergs s^{-1}}$ (G0.13-0.11) and $\sim 7.5 \times10^{32}
{\rm ergs s^{-1}}$ (point source) at the Galactic center distance of 8 kpc. The
morphological, spectral, and luminosity properties strongly indicate that
G0.13-0.11 represents the leading-edge of a pulsar wind nebula, produced by a
pulsar (point source) moving in a strong magnetic field environment. The main
body of this pulsar wind nebula is likely traced by a bow-shaped radio feature,
which is apparently bordered by G0.13-0.11 and is possibly associated with the
prominent nonthermal radio filaments of the Radio Arc. We speculate that young
pulsars may be responsible for various unique nonthermal filamentary radio and
X-ray features observed in the Galactic center region.
