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 overabundant relative to the solar values. Gaussian emission lines at ∼4 keV and ∼7 keV are detected. The ∼4 keV line is consistent with K-emission lines from 44 Ca and/or 44 Sc whereas the ∼7 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 ∼1.5 arcmin 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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