Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D
8 affiliations
- 1Western Sydney University
- 2Gifu University
- 3Dominion Astrophysical Observatory
- 4University of Baghdad
- 5Faculty of Mathematics, University of Belgrade
- 6Isaac Newton Institute of Chile
- 7Commonwealth Scientific and Industrial Research Organisation
- 8Astronomical Observatory
Abstract
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 1.2 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, with a maximum of ∼ 338 rad m. We estimate a constant partition magnetic field of ∼90 μG and a minimum energy of 3 × 10 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.
Versions
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BibTeX
@article{alsaberi2026radio,
title = {{Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D}},
author = {Rami Z. E. Alsaberi and Zachary J. Smeaton and Miroslav D. Filipovic and Roland Kothes and Hidetoshi Sano and Ahmed H. Abdullah and Dejan Urosevic and Sanja Lazarevic},
journal = {The Open Journal of Astrophysics},
year = {2026},
month = oct,
doi = {10.33232/001c.172272},
url = {https://astro.theoj.org/article/172272-radio-continuum-study-of-one-of-the-brightest-large-magellanic-cloud-supernova-remnants-n-132d},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Radio Continuum Study of One of the Brightest Large Magellanic Cloud Supernova Remnants N 132D
AU - Rami Z. E. Alsaberi
AU - Zachary J. Smeaton
AU - Miroslav D. Filipovic
AU - Roland Kothes
AU - Hidetoshi Sano
AU - Ahmed H. Abdullah
AU - Dejan Urosevic
AU - Sanja Lazarevic
PY - 2026
DA - 2026/10/09
JO - The Open Journal of Astrophysics
DO - 10.33232/001c.172272
UR - https://astro.theoj.org/article/172272-radio-continuum-study-of-one-of-the-brightest-large-magellanic-cloud-supernova-remnants-n-132d
AB - 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 1.2 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, with a maximum of ∼ 338 rad m. We estimate a constant partition magnetic field of ∼90 μG and a minimum energy of 3 × 10 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.
SN - 2565-6120
ER -