Abstract G284. 3-1. 8 is a supernova remnant with a radio shell and thermal X-ray emission. Located near its center is the gamma-ray binary 1FGL J1018. 6−5856, although the physical association between the two systems is not clear yet. Our X-ray spectroscopy with Suzaku reveals that G284. 3-1. 8 and 1FGL J1018. 6-5856 have compatible absorption column densities of NH = 6 --7 10^21~cm^-2, indicating that the two systems have similar distances. The actual distance is determined as 3 kpc using ^12CO (J=1 --0) data obtained with NANTEN. The X-ray spectrum of G284. 3-1. 8 shows a strong K-shell emission line of Mg, confirming the earlier claim that the SNR is one of the few Mg-rich SNRs. Comparing recent stellar models taking into account the “shell merger” processes, we find that the obtained Mg-to-Ne mass ratio of MMg/MNe = 0. 73^+0. 07-₀. ₀₃ and Si-to-Mg mass ratio of MSi/MMg = 0. 44 0. 03 suggest a supernova explosion that would have left a neutron star. The characteristics of 1FGL J1018. 6-5856, on the other hand, are better explained with a model in which its compact object is neutron star. The present results, therefore, would suggest a possible scenario where G284. 3-1. 8 and 1FGL J1018. 6-5856 are both remnants of a common supernova explosion, although further observational tests are necessary.
Terano et al. (Mon,) studied this question.