YOUNG ENERGETIC PSR J1617-5055, ITS NEBULA, AND TEV SOURCE HESS J1616-508

We observed the young 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 similar to 1' from the pulsar. Deconvolution and reconstruction of the image reveal a brighter compact PWN component of similar to 1 '' size. The total PWN luminosity in the 0.5-8 keV band, L-pwn = (3.2-3.7) x 10(33) erg s(-1) for d = 6.5 kpc, is a fraction of 2 x 10(-4) of the pulsar's spin-down power (E) over dot 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, L-pwn similar to 4L(psr). The pulsar's spectrum can be described by an absorbed power law with n(H) approximate to 3.5 x 10(22) cm(-2) and Gamma approximate to 1.1, harder than any other pulsar spectrum reliably measured in the soft X-ray band. This nonthermal emission is approximate to 50% pulsed, with 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' 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 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 supernova remnant or a star forming region, while some fraction of the TeV emission still may be attributed to the PWN around PSR J1617-5055.