%0 Journal Article %T Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512−6707 in the Large Magellanic Cloud %+ Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen %+ Western Sydney University %+ Cerro Tololo Inter-American Observatory %+ Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)) %+ Max-Planck-Institut für Extraterrestrische Physik (MPE) %A Kavanagh, P. J. %A Sasaki, M. %A Bozzetto, L. M. %A Points, S. D. %A Filipović, M. D. %A Maggi, P. %A Haberl, F. %A Crawford, E. J. %< avec comité de lecture %@ 0004-6361 %J Astronomy and Astrophysics - A&A %I EDP Sciences %V 583 %P A121 %8 2015-11 %D 2015 %R 10.1051/0004-6361/201526987 %K ISM: supernova remnants %K Magellanic Clouds %K X-rays: ISM %Z Physics [physics]/Astrophysics [astro-ph]Journal articles %X Aims. We present a multi-frequency study of the supernova remnant MCSNR J0512−6707 in the Large Magellanic Cloud.Methods. We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio polarisation and magnetic field orientation, and performed an X-ray spectral analysis.Results. We estimated the remnant’s size to be 24.9 ( ± 1.5) × 21.9 ( ± 1.5) pc, with the major axis rotated ~29° east of north. Radio polarisation images at 3 cm and 6 cm indicate a higher degree of polarisation in the northwest and southeast tangentially oriented to the SNR shock front, indicative of an SNR compressing the magnetic field threading the interstellar medium. The X-ray spectrum is unusual as it requires a soft (~0.2 keV) collisional ionisation equilibrium thermal plasma of interstellar medium abundance, in addition to a harder component. Using our fit results and the Sedov dynamical model, we showed that the thermal emission is not consistent with a Sedov remnant. We suggested that the thermal X-rays can be explained by MCSNR J0512−6707 having initially evolved into a wind-blown cavity and is now interacting with the surrounding dense shell. The origin of the hard component remains unclear. We could not determine the supernova type from the X-ray spectrum. Indirect evidence for the type is found in the study of the local stellar population and star formation history in the literature, which suggests a core-collapse origin.Conclusions. MCSNR J0512−6707 likely resulted from the core-collapse of high mass progenitor which carved a low density cavity into its surrounding medium, with the soft X-rays resulting from the impact of the blast wave with the surrounding shell. The unusual hard X-ray component requires deeper and higher spatial resolution radio and X-ray observations to confirm its origin. %G English %2 https://cea.hal.science/cea-01383761/document %2 https://cea.hal.science/cea-01383761/file/aa26987-15.pdf %L cea-01383761 %U https://cea.hal.science/cea-01383761 %~ CEA %~ INSU %~ UNIV-PARIS7 %~ CNRS %~ DSM-IRFU %~ IRFU-AIM %~ CEA-DRF %~ UNIV-PARIS %~ UP-SCIENCES %~ GS-PHYSIQUE