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arXiv · 0812.2186

Exploring the X-ray emission properties of the supernova remnant G67.7+1.8 and its central X-ray sources

C. Y. Hui·W. Becker
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Abstract

We have studied the supernova remnant G67.7+1.8 with the Chandra X-ray observatory. The remnant's X-ray morphology correlates well with the double-arc structure seen at radio wavelength. The X-ray spectra of the northern and southern rim of G67.7+1.8 exhibit emission line features of highly ionized metals, which suggests that most of the observed X-rays originate in a thermal plasma. We find magnesium, silicon, and sulphur are overabundant relative to the solar values. Gaussian emission lines at $\sim4$ keV and $\sim7$ keV are detected. The $\sim4$ keV line is consistent with K-emission lines from $^{44}$Ca and/or $^{44}$Sc whereas the $\sim7$ keV line feature may arise from unresolved Fe-K lines. Chandra's sub-arcsecond angular resolution allowed us to detect four faint point sources located within $\sim1.5$ arc-minutes of the geometrical remnant center. Among these objects, CXOU195424.75+312824.9 and CXOU195429.82+312834.1 do not have optical counterparts, leaving them as candidates for a possible compact stellar remnant.

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C. Y. Hui, W. Becker. 2008-12-11. Exploring the X-ray emission properties of the supernova remnant G67.7+1.8 and its central X-ray sources. https://doi.org/10.1051/0004-6361%3A200810789

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