Multifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902

L. M. Bozzetto*, P. J. Kavanagh, P. Maggi, M. D. Filipović, M. Stupar, Q. A. Parker, W. A. Reid, M. Sasaki, F. Haberl, D. Urošević, J. Dickel, R. Sturm, R. Williams, M. Ehle, R. Gruendl, Y. H. Chu, S. Points, E. J. Crawford

*Corresponding author for this work

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We present a detailed radio, X-ray and optical study of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR) which we denote as MCSNR J0508-6902. Observations from the Australia Telescope Compact Array (ATCA) and the XMM-Newton X-ray observatory are complemented by deep Hα images and Anglo-Australian Telescope AAOmega spectroscopic data to study the SNR shell and its shock ionization. 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 ~74 pc × 57 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-fitting temperature to the shell X-ray emission κT = 0.41 +0.05-0.06 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 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 ~28 μG, a value typical of older SNRs and consistent with other analyses which also infer an older remnant.

Original languageEnglish
Pages (from-to)1110-1124
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Issue number1
Publication statusPublished - Mar 2014

Bibliographical note

Copyright 2014 The Authors. First published in Monthly Notices of the Royal Astronomical Society, 439(1), pp. 1110-1124. The original publication is available at, published by Oxford University Press. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.


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