Modeling The Broadband High Energy Emission Spectrum Of PWN Associated With The PSR J1617-5055

Details Modeling The Broadband High Energy Emission Spectrum Of PWN Associated With The PSR J1617-5055 Modeling The Broadband High Energy Emission Spectrum Of PWN Associated With The PSR J1617-5055

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21430904k&link_type=abstract

American Astronomical Society, AAS Meeting #214, #309.04; Bulletin of the American Astronomical Society, Vol. 41, p.738

Astronomy and Astrophysics

Astronomy

Scientific paper

The ground-based Cherenkov detectors discovered, in a survey of the Galactic plane, a population of TeV γ-ray sources that are still without definitive counterparts at longer wavelengths. For a number of these sources, a pulsar is an evident association, which is often located within an extended region of the TeV γ-ray emission. These particular γ-ray sources are promising candidates for yet not resolved pulsar wind nebulae. Recently, an X-ray emitting PWN, CXOU J161729.3-505512, has been detected for one of those sources, i.e., HESS J1616-508, with Chandra, BeppoSAX, XMM, and INTEGRAL. This extended X-ray source is associated with the pulsar PSR J1617-5055, which could be the underlying engine of the unidentified TeV γ-ray source. Here we present the modeling of the broadband spectral energy distribution of this object detected in the X-rays and TeV γ rays. Results of detailed modeling in the multi-zone approach strongly support the interpretation of the TeV emission as a hallmark of the PWN powered by the energetic pulsar.

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