Multiwavelength study of the newly confirmed supernova remnant MCSNR J0527−7104 in the Large Magellanic Cloud
Multiwavelength study of the newly confirmed supernova remnant MCSNR J0527−7104 in the Large Magellanic Cloud
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大麦哲伦星云中新确认的超新星遗迹 MCSNR J0527â7104 的多波长研究
DOI：
10.1051/0004-6361/201220431
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发表时间：
2013
影响因子：
6.5
通讯作者：
Pietsch
中科院分区：
文献类型：
--
作者：
Kavanagh;Sasaki;Points;Filipović;Bozzetto;Crawford;Haberl;Pietsch
背景大麦哲伦星云 (LMC) 拥有丰富多样的超新星遗迹 (SNR)。需要光学、X 射线和射电观测来识别这些 SNR，并确定导致观察到的大量物理特征的各种过程。目的在本文中，我们试图通过用光学和射电观测补充这些 X 射线数据来确认 ROSAT 在 X 射线中识别的候选 SNR [HP99] 1234 是否为真正的 SNR。方法来自麦哲伦云发射线勘测 (MCELS) 的光学数据和来自除了 ROSAT X 射线数据之外，还使用莫隆格洛天文台合成望远镜 (MOST) 对该候选 SNR 进行多波长形态分析。结果在光学中检测到增强的 [S ii] 发射的近似椭圆体壳，这是典型的 SNR ([S ii]/Hα> 0.4)。这种增强在位置上与 λ= 36 cm 处的微弱射电发射一致。利用现有数据，我们估计残骸的大小为 ~5.1′ × 4.0′ (~75 pc × 59 pc)。然而，由于其末端缺乏光学和无线电发射以及 X 射线数据的分辨率较差，沿主轴的测量有些不确定。假设该信噪比处于谢多夫相，并采用在附近 H ii 区域测量的环境质量密度 1.2 × 10-25g cm-3，则针对 1051erg 的规范初始爆炸能量计算出约 25 kyr 的年龄估计。然而，由于所采用参数的不确定性，应谨慎对待这一年龄估计。对当地恒星群的分析表明，Ia 型事件是该 SNR 的前兆，然而，由于前身可能是一颗失控的大质量恒星，因此不能排除核心塌缩机制。结论通过检测到 X 射线、射电和增强的 [S ii] 的显着光线发射，该天体被确认为 SNR，我们为其分配了标识符 MCSNR J0527−7104。
ContextThe Large Magellanic Cloud (LMC) hosts a rich and varied population of supernova remnants (SNRs). Optical, X-ray, and radio observations are required to identify these SNRs, as well as to ascertain the various processes responsible for the large array of physical characteristics observed.AimsIn this paper we attempted to confirm the candidate SNR [HP99] 1234, identified in X-rays with ROSAT, as a true SNR by supplementing these X-ray data with optical and radio observations.MethodsOptical data from the Magellanic Cloud Emission Line Survey (MCELS) and new radio data from the Molonglo Observatory Synthesis Telescope (MOST), in addition to the ROSAT X-ray data, were used to perform a multiwavelength morphological analysis of this candidate SNR.ResultsAn approximately ellipsoidal shell of enhanced [S ii] emission, typical of an SNR ([S ii]/Hα> 0.4), was detected in the optical. This enhancement is positionally coincident with faint radio emission atλ= 36 cm. Using the available data we estimated the size of the remnant to be ~5.1′ × 4.0′ (~75 pc × 59 pc). However, the measurement along the major-axis was somewhat uncertain due to a lack of optical and radio emission at its extremities and the poor resolution of the X-ray data. Assuming this SNR is in the Sedov phase and adopting the ambient mass density of 1.2 × 10-25g cm-3measured in a nearby H ii region, an age estimate of ~25 kyr was calculated for a canonical initial explosion energy of 1051erg. However, this age estimate should be treated cautiously due to uncertainties on the adopted parameters. Analysis of the local stellar population suggested a type Ia event as a precursor to this SNR, however, a core-collapse mechanism could not be ruled out due to the possibility of the progenitor being a runaway massive star.ConclusionsWith the detection of X-ray, radio and significant optical line emission with enhanced [S ii], this object was confirmed as an SNR to which we assign the identifier MCSNR J0527−7104.
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影响因子：
6.5
作者：
P. Maggi;F. Haberl;L. Bozzetto;M. Filipović;S. Points;You;M. Sasaki;W. Pietsch;R. Gruendl;J. Dickel;R. Smith;R. Sturm;E. Crawford;A. Horta
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DOI：
10.1086/431349
发表时间：
2005
期刊：
The Astrophysical Journal
影响因子：
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作者：
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DOI：
10.1086/422689
发表时间：
2004
期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
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C. Packham
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DOI：
10.1111/j.1365-2966.2008.13884.x
发表时间：
2008
影响因子：
4.8
作者：
G. Benedetto
通讯作者：
G. Benedetto
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影响因子：
6.5
作者：
Kavanagh;Sasaki;Points
通讯作者：
Points