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 { 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 0.38 d _ { 0.38 } kpc and a temperature of 61.7 \pm 3.0 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 .