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We observed the young energetic pulsar J1617-5055 with the Chandra ACISdetector for 60 ks. In addition to the pulsar, the X-ray images show a faintpulsar-wind nebula (PWN) seen up to ~1' from the pulsar. Deconvolution andreconstruction of the image reveal a brighter compact PWN component of ~1''size, possibly with a jet-torus morphology. The PWN spectrum fits an absorbedpower-law (PL) model with the photon index Gamma=1.5. The total PWN luminosityin the 0.5-8 keV band, L_{pwn}=3.2\times10^{33} ergs s^{-1} for d=6.5 kpc, is afraction of 2\times 10^{-4} of the pulsar's spin-down power and a fraction of0.2 of the pulsar's X-ray luminosity, which is a factor of 20 lower than onewould expect from an average empirical relation found for a sample of PWNeobserved with Chandra. The pulsar's spectrum can be described by an absorbed PLwith n_{H}=3.5\times10^{22} cm^{-2} and Gamma=1.1, harder than any other pulsarspectrum reliably measured in the soft X-ray band. This non-thermal emission is50% pulsed showing one peak per period. We have also investigated a possibleconnection between J1617 and the extended TeV source HESS J1616-508 whosecenter is located about 10' west of the pulsar. We find no preferentialextension of the X-ray PWN toward the TeV source. Therefore, the Chandra datado not provide conclusive evidence for PSR J1617-5055 and HESS J1616-508association. We have also analyzed archival X-ray, radio, and IR data on theHESS J1616-508 region and found traces of diffuse emission (resembling a shellin the radio) coinciding with the central part of HESS J1616-508. We speculatethat the TeV source may be multiple, with most of the emission coming from anunknown SNR or a star-forming region, while some fraction of the TeV emissionstill may be attributed to the J1617 PWN.

Young energetic PSR J1617-5055, its underluminous nebula and unidentified TeV source HESS J1616-508