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PSR J1809-1917 is a young ($\tau=51$ kyr) energetic($\dot{E}=1.8\times10^{36}$ erg s$^{-1}$) radio pulsar powering an X-ray pulsarwind nebula (PWN) that exhibits morphological variability. We report on theresults of a new monitoring campaign by the Chandra X-ray Observatory (CXO),carried out across 6 epochs with a $\sim$7-week cadence. The compact nebula canbe interpreted as a jet-dominated outflow along the pulsar's spin axis. Itsvariability can be the result of Doppler boosting in the kinked jet whose shapechanges with time (akin to the Vela pulsar jet). The deep X-ray image, composedof 405 ks of new and 131 ks of archival CXO data, reveals an arcminute-scaleextended nebula (EN) whose axis of symmetry aligns with both the axis of thecompact nebula and the direction toward the peak of the nearby TeV source HESSJ1809-193. The EN's morphology and extent suggest that the pulsar is likelymoving through the ambient medium at a transonic velocity. We also resolved afaint 7$'$-long nonthermal collimated structure protruding from the PWN. It ispossibly another instance of a "misaligned outflow" (also known as a "kineticjet") produced by high-energy particles escaping the PWN's confinement andtracing the interstellar magnetic field lines. Finally, taking advantage of the536 ks exposure, we analyzed the point sources in the J1809 field andclassified them using multiwavelength data. None of the classified sources inthe field can reasonably be expected to produce the extended TeV flux in theregion, suggesting that PSR J1809-1917 is indeed the counterpart to HESS/eHWCJ1809-193.

Chandra Monitoring of the J1809-1917 Pulsar Wind Nebula and Its Field