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Li et al. have used archival ASKAP data to study the Supernova Remnant
SNR B0532-67.5 in the Large Magellanic Cloud (LMC). SNR B0532-67.5
was first reported by Mathewson et al. in 1985, who noted the absence
of an associated optical shell structure, despite the presence of
nonthermal radio emission and X-ray source. The association of young,
bright OB stars, LH75, or NGC 2011, is projected within the boundary
of this SNR. Li et al. use optical photometric data to determine a
20--25 Myr population in LH75 and a younger population, less than 10
Myr old, to the southwest of LH75. They conclude that the SN
progenitor was probably a member of LH75 with an initial mass of about
15 solar masses. The SN probably exploded in an H I cavity excavated
by the energy feedback of LH75, with the low density of the ambient
medium prohibiting the formation of a visible nebular shell.
The figures above show the ASKAP 888 MHz data, overplotted with ASKAP contours (left)
and contours of a XMM smoothed X-ray image (right) showing a general consistency between
X-ray and radio images.
The paper has been published in the Astronomical Journal.
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