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HESS J1825-137: A pulsar wind nebula associated with PSR B1823-13?

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Funk,  Stefan
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Hinton,  James
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Citation

de Jager, O. C., Funk, S., & Hinton, J. (2005). HESS J1825-137: A pulsar wind nebula associated with PSR B1823-13? In B. S. Acharya, S. Gupta, P. Jagadeesan, A. Jain, S. Karthikeyan, S. Morris, et al. (Eds.), Proceedings of the 29th International Cosmic Ray Conference (pp. 239-242). Navy Nagar, Colaba, Mumbai, MH-400005: Tata Institute of Fundamental Research.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-8799-0
Abstract
HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the H.E.S.S. instrument in 2004. Both HESS J1825-137 and the X-ray pulsar wind nebula G18.0-0.7 (associated with the Vela-like pulsar PSR B1823-13) are offset south of the pulsar, which may be the result of the SNR expanding into an inhomogeneous medium. The TeV size (~35pc, for a distance of 4 kpc) is ~6 times larger than the X-ray size, which may be the result of propagation effects as a result of the longer lifetime of TeV emitting electrons, compared to the relatively short lifetime of keV synchrotron emitting electrons. The TeV photon spectral index of ~2.4 can also be related to the extended PWN X-ray synchrotron photon index of ~2.3, if this spectrum is dominated by synchrotron cooling. The anomalously large size of the pulsar wind nebula can be explained if the pulsar was born with a relatively large initial spindown power and braking index n~2, provided that the SNR expanded into the hot ISM with relatively low density (~0.003 cm-3).