The X-ray Halo of G21.5-0.9

Details The X-ray Halo of G21.5-0.9 The X-ray Halo of G21.5-0.9

2003-05-21

arxiv.org/abs/astro-ph/0305398v1

Astronomy and Astrophysics

Astrophysics

6 pages, 5 figures, Latex, txfonts cospar and natbib macro packages, to appear in "High Energy Studies of Supernova Remnants a

Scientific paper

10.1016/j.asr.2003.04.025

The emission of the plerion G21.5-0.9 appears more extended in X rays than in radio. This is an unexpected result because it would imply that short-lived X-ray electrons may reach distances even larger than radio electrons. Applying an empirical relationship between dust scattering optical depth and photoelectric column density, the measured column density leads to a large optical depth at 1 keV, of about 1. Therefore we investigate the hypothesis that the detected halo be an effect of dust scattering, re-analyzing an Cal/PV XMM-Newton observation of G21.5-0.9 and critically examining it in terms of a dust scattering model. We also present a spectral analysis of a prominent extended feature in the northern sector of the halo.

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