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

doi:10.1093/mnras/stu051

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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Abstract

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 language	English
Pages (from-to)	1110-1124
Number of pages	15
Journal	Monthly Notices of the Royal Astronomical Society
Volume	439
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stu051
Publication status	Published - 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 http://doi.org/10.1093/mnras/stu051, 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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Bozzetto, L. M., Kavanagh, P. J., Maggi, P., Filipović, M. D., Stupar, M., Parker, Q. A., Reid, W. A., Sasaki, M., Haberl, F., Urošević, D., Dickel, J., Sturm, R., Williams, R., Ehle, M., Gruendl, R., Chu, Y. H., Points, S., & Crawford, E. J. (2014). Multifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902. Monthly Notices of the Royal Astronomical Society, 439(1), 1110-1124. https://doi.org/10.1093/mnras/stu051

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

abstract = "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.",

author = "Bozzetto, {L. M.} and Kavanagh, {P. J.} and P. Maggi and Filipovi{\'c}, {M. D.} and M. Stupar and Parker, {Q. A.} and Reid, {W. A.} and M. Sasaki and F. Haberl and D. Uro{\v s}evi{\'c} and J. Dickel and R. Sturm and R. Williams and M. Ehle and R. Gruendl and Chu, {Y. H.} and S. Points and Crawford, {E. J.}",

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 http://doi.org/10.1093/mnras/stu051, 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.",

year = "2014",

month = mar,

doi = "10.1093/mnras/stu051",

language = "English",

volume = "439",

pages = "1110--1124",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

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Bozzetto, LM, Kavanagh, PJ, Maggi, P, Filipović, MD, Stupar, M, Parker, QA, Reid, WA, Sasaki, M, Haberl, F, Urošević, D, Dickel, J, Sturm, R, Williams, R, Ehle, M, Gruendl, R, Chu, YH, Points, S & Crawford, EJ 2014, 'Multifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902', Monthly Notices of the Royal Astronomical Society, vol. 439, no. 1, pp. 1110-1124. https://doi.org/10.1093/mnras/stu051

TY - JOUR

T1 - Multifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902

AU - Bozzetto, L. M.

AU - Kavanagh, P. J.

AU - Maggi, P.

AU - Filipović, M. D.

AU - Stupar, M.

AU - Parker, Q. A.

AU - Reid, W. A.

AU - Sasaki, M.

AU - Haberl, F.

AU - Urošević, D.

AU - Dickel, J.

AU - Sturm, R.

AU - Williams, R.

AU - Ehle, M.

AU - Gruendl, R.

AU - Chu, Y. H.

AU - Points, S.

AU - Crawford, E. J.

N1 - 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 http://doi.org/10.1093/mnras/stu051, 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.

PY - 2014/3

Y1 - 2014/3

N2 - 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.

AB - 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.

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DO - 10.1093/mnras/stu051

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

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