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We present a study of the supernova remnant MCSNR J0512-6707 in the LargeMagellanic Cloud. We used new data from XMM-Newton to characterise the X-rayemission and data from the Australian Telescope Compact Array, the MagellanicCloud Emission Line Survey, and Spitzer to gain a picture of the environmentinto which the remnant is expanding. We performed a morphological study,determined radio polarisation and magnetic field orientation, and performed anX-ray spectral analysis. We estimated the its size to be 24.9 (\pm1.5) x 21.9(\pm1.5) pc, with the major axis rotated ~29 deg east of north. Radiopolarisation at 3 cm and 6 cm indicate a higher degree of polarisation in theNW and SE tangentially oriented to the SNR shock front, indicative of an SNRcompressing the magnetic field threading the interstellar medium. The X-rayspectrum is unusual as it requires a soft (~0.2 keV) CIE thermal plasma ofinterstellar medium abundance, in addition to a harder component. Using ourresults and the Sedov dynamical model, we showed that this emission is notconsistent with a Sedov remnant. We suggested that the thermal X-rays can beexplained by MCSNR J0512-6707 having initially evolved into a wind-blown cavityand is now interacting with the surrounding dense shell. The origin of the hardcomponent remains unclear. We could not determine the supernova type from theX-ray spectrum. Indirect evidence was found in the study of the local stellarpopulation and star formation history in the literature, which suggests acore-collapse origin. MCSNR J0512-6707 likely resulted from the core-collapseof high mass progenitor which carved a low density cavity into its surroundingmedium, with the soft X-rays resulting from the impact of the blast wave withthe surrounding shell. The unusual hard X-ray component requires deeper andhigher spatial resolution radio and X-ray observations to confirm its origin.

Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud