We observed the young energetic pulsar J1617 - 5055 with the Chandra ACIS detector for 60 ks .
In addition to the pulsar , the X-ray images show a faint pulsar-wind nebula ( PWN ) seen up to \sim 1 ^ { \prime } from the pulsar .
Deconvolution and reconstruction of the image reveal a brighter compact PWN component of \sim 1 ^ { \prime \prime } size , possibly with a jet-torus morphology .
The PWN spectrum fits an absorbed power-law ( PL ) model with the photon index \Gamma \approx 1.5 .
The total PWN luminosity in the 0.5–8 keV band , L _ { pwn } = 3.2 \times 10 ^ { 33 } ergs s ^ { -1 } for d = 6.5 kpc , is a fraction of 2 \times 10 ^ { -4 } of the pulsar ’ s spin-down power \dot { E } and a fraction of 0.2 of the pulsar ’ s X-ray luminosity , which is a factor of 20 lower than one would expect from an average empirical relation found for a sample of PWNe observed with Chandra .
The pulsar ’ s spectrum can be described by an absorbed PL with n _ { H } \approx 3.5 \times 10 ^ { 22 } cm ^ { -2 } and \Gamma \approx 1.1 , harder than any other pulsar spectrum reliably measured in the soft X-ray band .
This non-thermal emission is \approx 50 \% pulsed showing one peak per period .
We have also investigated a possible connection between J1617 and the extended TeV source HESS J1616–508 whose center is located 10 ^ { \prime } west of the pulsar .
We find no preferential extension of the X-ray PWN toward the TeV source .
Therefore , the Chandra data do not provide conclusive evidence for PSR J1617–5055 and HESS J1616–508 association .
We have also analyzed archival X-ray , radio , and IR data on the HESS J1616–508 region and found traces of diffuse emission ( resembling a shell in the radio ) coinciding with the central part of HESS J1616–508 .
We speculate that the TeV source may be multiple , with most of the emission coming from an unknown SNR or a star-forming region , while some fraction of the TeV emission still may be attributed to the J1617 PWN .