  We obtained six observations of PSR J1741-2054 using the $Chandra$ ACIS-S
detector totaling $\sim$300 ks. By registering this new epoch of observations
to an archival observation taken 3.2 years earlier using X-ray point sources in
the field of view, we have measured the pulsar proper motion at $\mu =109 \pm
10 {\rm mas\ yr}^{-1}$ in a direction consistent with the symmetry axis of the
observed H$\alpha$ nebula. We investigated the inferred past trajectory of the
pulsar but find no compelling association with OB associations in which the
progenitor may have originated. We confirm previous measurements of the pulsar
spectrum as an absorbed power law with photon index $\Gamma$=2.68$\pm$0.04,
plus a blackbody with an emission radius of (4.5$^{+3.2}_{-2.5})d_{0.38}$ km,
for a DM-estimated distance of $0.38d_{0.38}$ kpc and a temperature of
$61.7\pm3.0$ eV. Emission from the compact nebula is well described by an
absorbed power law model with a photon index of $\Gamma$ = 1.67$\pm$0.06, while
the diffuse emission seen as a trail extending northeast of the pulsar shows no
evidence of synchrotron cooling. We also applied image deconvolution techniques
to search for small-scale structures in the immediate vicinity of the pulsar,
but found no conclusive evidence for such structures.

High Energy Astrophysical Phenomena