2015ApJ...802...68A

We obtained six observations of PSR J1741-2054 using the Chandra ACIS-S detector totaling ∼300 ks. By registering this new epoch of observations to an archival observation taken 3.2 yr earlier using X-ray point sources in the field of view, we have measured the pulsar proper motion at µ = 109 ± 10 mas/yr in a direction consistent with the symmetry axis of the observed Hα 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 Γ = 2.68±0.04, plus a blackbody with an emission radius of (4.5_–2.5^+3.2)d_0,38 km, for a DM-estimated distance of kpc and a temperature of 61.7±3.0 eV. Emission from the compact nebula is well described by an absorbed power law model with a photon index of Γ = 1.67±0.06, while the diffuse emission seen as a trail extending northeast of the pulsar shows no evidence of synchrotron 0.38d_0.38 kpc 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.