Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnant N 132D

We present a new radio continuum study of the Large Magellanic Cloud supernova remnant N 132D using observations from the Australia Telescope Compact Array (ATCA) and MeerKAT. The radio morphology shows a clear spatial correlation with the X-ray emission in the central and left regions of the remnant, as well as in the right portion of the shell, indicating a close connection between the thermal and non-thermal plasma components. Polarisation measurements reveal predominantly radial magnetic fields, with mean fractional polarisations of 1.3 per cent, 3.0 per cent, and 4.0 per cent at 2100, 5500, and 9000 MHz, respectively. There is also a complex structure seen in the Faraday Depth spectrum, showing a double-peaked structure which indicates regions with differing magnetisation properties or varying magnetic field geometry. The rotation measure derived from ATCA data has an average value of ∼ 2 rad m\({\mathstrut}^{−2}\), with a maximum of ∼ 338 rad m\({\mathstrut}^{−2}\). We estimate a constant partition magnetic field of ∼90 μG and a minimum energy of 3 × 10\({\mathstrut}^{50}\) erg, which is in a constant partition between the energy density of electrons and the energy density of the magnetic field. The integrated radio spectrum follows a power law with a spectral index of −0.74 ± 0.01. These results provide new constraints on the magnetic field structure and energetic properties of of N 132D and offer insight into particle acceleration and shock evolution in young supernova remnants.