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

TitleMultifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902
Authors
KeywordsRadio continuum: ISM
Magellanic clouds
ISM: Supernova remnants
X-rays: ISM
Issue Date2014
Citation
Monthly Notices of the Royal Astronomical Society, 2014, v. 439, n. 1, p. 1110-1124 How to Cite?
AbstractWe 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. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Persistent Identifierhttp://hdl.handle.net/10722/209023
ISSN
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DC FieldValueLanguage
dc.contributor.authorBozzetto, Luke M.-
dc.contributor.authorKavanagh, Patrick J.-
dc.contributor.authorMaggi, P.-
dc.contributor.authorFilipovíc, Miroslav D.-
dc.contributor.authorStupar, Milorad-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSasaki, Manami-
dc.contributor.authorHaberl, Frank W.-
dc.contributor.authorUrǒsević, Dejan-
dc.contributor.authorDickel, John R.-
dc.contributor.authorSturm, Richard-
dc.contributor.authorWilliams, Robert J.-
dc.contributor.authorEhle, Matthias-
dc.contributor.authorGruendl, Robert A.-
dc.contributor.authorChu, Youhua-
dc.contributor.authorPoints, Sean D.-
dc.contributor.authorCrawford, Evan J.-
dc.date.accessioned2015-03-23T02:31:11Z-
dc.date.available2015-03-23T02:31:11Z-
dc.date.issued2014-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2014, v. 439, n. 1, p. 1110-1124-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/209023-
dc.description.abstractWe 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. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectRadio continuum: ISM-
dc.subjectMagellanic clouds-
dc.subjectISM: Supernova remnants-
dc.subjectX-rays: ISM-
dc.titleMultifrequency study of a new fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1093/mnras/stu051-
dc.identifier.scopuseid_2-s2.0-84894670217-
dc.identifier.volume439-
dc.identifier.issue1-
dc.identifier.spage1110-
dc.identifier.epage1124-
dc.identifier.eissn1365-2966-

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