Young Energetic PSR J1617-5055, Its Underluminous Nebula, And TeV Source HESS J1616-508

Details Young Energetic PSR J1617-5055, Its Underluminous Nebula, And TeV Source HESS J1616-508 Young Energetic PSR J1617-5055, Its Underluminous Nebula, And TeV Source HESS J1616-508

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.1207p&link_type=abstract

American Astronomical Society, HEAD meeting #10, #12.07

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A Chandra ACIS observation of the young energetic pulsar J1617-5055 revealed a faint pulsar wind nebula (PWN) extending up to 1' from the pulsar. The PWN possibly has a very compact, brighter component of 2'' size. The non-thermal spectrum of the compact PWN fits an absorbed power-law (PL) model with the photon index Gamma=1.47+/-0.24, which increases to 1.65+/-0.2 farther away from the pulsar. The luminosity of the whole PWN is just 20% of the pulsar luminosity, factor of 20 lower than that of a typical PWN. This suggests that the radiative efficiencies of PWNe can be strongly affected by ``hidden'' parameters other than the pulsar's spindown energy loss rate. The high S/N pulsar spectrum is surprisingly hard, Gamma=1.14+/-0.06,harder than any other pulsar spectrum reliably measured in the X-ray band. We have also investigated a possible connection between PSR J1617-5055 and the extended TeV source HESS J1616-508, centered 14' west of the pulsar. As we found no preferential extension of the X-ray PWN toward the TeV source, we cannot confirm the proposed association between these two objects. However, archival X-ray, radio and IR data show diffuse emission (resembling a shell in the radio) coinciding with the central part of HESS J1616-508. We speculate that HESS J1616-508 may be a multiple source, with most of the emission coming from an unknown SNR or a star-forming region, while some fraction of the TeV emission still might be attributed to the J1617-5055 PWN.

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