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Title:
Young Energetic PSR J1617-5055, Its Nebula, and TeV Source HESS J1616-508
Authors:
Kargaltsev, O.; Pavlov, G. G.; Wong, J. A.
Affiliation:
AA(Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL 32611, USA ; The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA; ), AB(The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA ), AC(The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA)
Publication:
The Astrophysical Journal, Volume 690, Issue 1, pp. 891-901 (2009). (ApJ Homepage)
Publication Date:
01/2009
Origin:
IOP
ApJ Keywords:
ISM: individual: HESS J1616–508, pulsars: individual: PSR J1617–5055, stars: neutron, X-rays: ISM
DOI:
10.1088/0004-637X/690/1/891
Bibliographic Code:
2009ApJ...690..891K

Abstract

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 ~1' from the pulsar. Deconvolution and reconstruction of the image reveal a brighter compact PWN component of ~1'' size. The total PWN luminosity in the 0.5-8 keV band, L pwn = (3.2-3.7) × 1033 erg s-1 for d = 6.5 kpc, is a fraction of 2 × 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, L pwn ~ 4L psr. The pulsar's spectrum can be described by an absorbed power law with n H ≈ 3.5 × 1022 cm-2 and Γ ≈ 1.1, harder than any other pulsar spectrum reliably measured in the soft X-ray band. This nonthermal emission is ≈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.
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