We present a detailed radio , X-ray and optical study of a newly discovered Large Magellanic Cloud ( LMC ) supernova remnant ( SNR ) which we denote MCSNRÂ J0508–6902 .
Observations from the Australian Telescope Compact Array ( ATCA ) and the XMM-Newton  X-ray observatory are complemented by deep H \alpha images and Anglo Australian Telescope AAOmega spectroscopic data to study the SNR shell and its shock-ionisation .
Archival data at other wavelengths are also examined .
The remnant follows a filled-in shell type morphology in the radio–continuum and has a size of \sim 74Â pc \times 57Â pc at the LMC distance .
The X-ray emission exhibits a faint soft shell morphology with Fe-rich gas in its interior – indicative of a Type Ia origin .
The remnant appears to be mostly dissipated at higher radio-continuum frequencies leaving only the south-eastern limb fully detectable while in the optical it is the western side of the SNR shell that is clearly detected .
The best-fit temperature to the shell X-ray emission ( kT = 0.41 ^ { +0.05 } _ { -0.06 } Â keV ) is consistent with other large LMC SNRs .
We determined an O/Fe ratio of < 21 and an Fe mass of 0.5–1.8 M _ { \sun } in the interior of the remnant , both of which are consistent with the Type Ia scenario .
We find an equipartition magnetic field for the remnant of \sim 28Â \mu G , a value typical of older SNRs and consistent with other analyses which also infer an older remnant .