XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud
XMM-Newton study of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud
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对 30 Doradus C 和大麦哲伦星云中新发现的 MCSNR J0536â6913 的 XMM-Newton 研究
DOI：
10.1051/0004-6361/201424354
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发表时间：
2015
影响因子：
6.5
通讯作者：
Haberl
中科院分区：
文献类型：
--
作者：
Kavanagh;Sasaki;Bozzetto;Filipović;Points;Haberl
目的详细研究大麦哲伦星云中的超新星遗迹MCSNRJ0536-6913和超泡30DOR C。方法利用XMM-Newtondata(耀斑过滤曝光时间分别为420kS EPIC-PN、556KS EPIC-MOS1、614KS EPIC-MoS2)对该区域的热X射线辐射进行了表征。文中还对非热X射线发射进行了分析，并结合文献中提出的发射机制进行了讨论。这些数据得到了钱德拉的X射线数据、麦哲伦云发射线调查的光学数据以及澳大利亚望远镜紧凑型阵列和莫龙格罗天文台综合望远镜的射电数据的补充。结果发现最亮的30度或更高温度的热发射与一颗新的超新星遗迹有关，−J0536 MCSNR6913。对MCSNRJ0536−6913的X射线能谱分析表明，它是一个以喷出物为主的残留物，有O，Ne，Mg和Si谱线，总X射线光度为0.3−，10keV的X射线光度为~8×1034erg S-1。根据得到的喷射物丰度比，我们确定恒星前体的质量为~18m⊙或高达≳40m⊙，尽管光谱拟合受到简化假设的影响(例如，均匀的温度和良好混合的喷射物)。超泡的热发射显示出α过程元素的浓缩，这是最近与超泡壳层发生核崩塌信噪比相互作用的证据。我们在30dor C期间探测到了非热X射线发射，其中最亮的区域与Hα和射电壳层高度相关。建立了30Dor C东北壳层的非热谱能量分布，与指数截止同步辐射模型符合得最好。结论30Dor C壳层的热X射线发射非常复杂，由壳层东部的大尺度超气泡发射组成，最亮的发射来自−6913。观测到超泡壳层的非热谱能量分布为滚落这一事实，进一步证明了30Dor C的非热X射线发射是同步辐射的起源。
AimsWe present a detailed study of the superbubble 30 Dor C and the newly identified supernova remnant MCSNR J0536-6913 in the Large Magellanic Cloud.MethodsAll availableXMM-Newtondata (flare-filtered exposure times of 420 ks EPIC-pn, 556 ks EPIC-MOS1, 614 ks EPIC-MOS2) were used to characterise the thermal X-ray emission in the region. An analysis of the non-thermal X-ray emission is also presented and discussed in the context of emission mechanisms previously suggested in the literature. These data are supplemented by X-ray data fromChandra, optical data from the Magellanic Cloud Emission Line Survey, and radio data from the Australia Telescope Compact Array and the Molonglo Observatory Synthesis Telescope.ResultsThe brightest thermal emission towards 30 Dor C was found to be associated with a new supernova remnant, MCSNR J0536−6913. X-ray spectral analysis of MCSNR J0536−6913 suggested an ejecta-dominated remnant with lines of O, Ne, Mg, and Si, and a total 0.3−10 keV X-ray luminosity of ~8 × 1034erg s-1. Based on derived ejecta abundance ratios, we determined the mass of the stellar progenitor to be either ~18M⊙or as high as ≳40M⊙, though the spectral fits were subject to simplifying assumptions (e.g., uniform temperature and well-mixed ejecta). The thermal emission from the superbubble exhibited enrichment byα-process elements, evidence for a recent core-collapse SNR interaction with the superbubble shell. We detected non-thermal X-ray emission throughout 30 Dor C, with the brightest regions being highly correlated with the Hαand radio shells. We created a non-thermal spectral energy distribution for the north-eastern shell of 30 Dor C which was best-fit with an exponentially cut-off synchrotron model.ConclusionsThermal X-ray emission from 30 Dor C is very complex, consisting of a large scale superbubble emission at the eastern shell wall with the brightest emission due to MCSNR J0536−6913. The fact that the non-thermal spectral energy distribution of the superbubble shell was observed to roll-off is further evidence that the non-thermal X-ray emission from 30 Dor C is synchrotron in origin.
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影响因子：
4.8
作者：
L. Bozzetto;M. Filipović;D. Urošević;R. Kothes;E. Crawford
通讯作者：
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大麦哲伦星云中超新星遗迹的 X 射线光谱分类
DOI：
--
发表时间：
1982
期刊：
影响因子：
--
作者：
D. H. Clark;I. Tuohy;M. Dopita;D. Mathewson;K. Long;A. Szymkowiak;J. Culhane
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DOI：
10.1086/345611
发表时间：
2002
期刊：
The Astrophysical Journal Letters
影响因子：
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作者：
S. Wolk;T. Bourke;Randall K. Smith;B. Spitzbart;J. Alves
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提交给《天体物理学杂志快报》预印本排版，使用 L ATEX 样式 emulateapj v. 25/04/01 0103−72.6：小麦哲伦星云中新的富氧超新星遗迹
DOI：
--
发表时间：
2003
期刊：
影响因子：
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作者：
G. Bertaccini;G. Coruzzi
通讯作者：
G. Coruzzi
小麦哲伦星云的 X 射线巡天
DOI：
10.1086/158641
发表时间：
1981
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. Seward;Melanie Mitchell
通讯作者：
Melanie Mitchell