  One of the most unique phenomena in the Galactic center region is the
existence of numerous long and narrow filamentary structures within a few
hundred parsecs of Sgr A$^{\star}$. While more than one than one hundred radio
filaments have been revealed by MeerKAT, about two dozens X-ray filaments have
been discovered so far. In this article, we report our analysis on the deep
Chandra and NuSTAR observations of a non-thermal X-ray filament, G0.13-0.11,
which is located adjacent to the Radio arc. Chandra revealed a unique
morphology of G0.13-0.11, which is an elongated (0.1 pc in width and 3.2 pc in
length) structure slightly bended towards the Radio arc. A pulsar candidate
($\Gamma \sim 1.4$) is detected in the middle of the filament, with a tail of
diffuse non-thermal X-ray emission on one side of the filament. The filament is
detected by NuSTAR up to 79 keV, with the hard X-ray centroid consistent with
the pulsar candidate. We found that the X-ray intensity decays along the
filament farther away from the pulsar candidate, dropping to half of its peak
value at 2.2 pc away. This system is mostly likely a Pulsar Wind Nebula
interacting with ambient interstellar magnetic field, where the filaments are
kinetic jets from PWN as recently proposed. The nature of this filament adds to
complex origin of the X-ray filaments, which serve as powerful tools to probe
local and global powerful particle accelerators in the Galactic center.
