The supernova remnant population of the Small Magellanic Cloud
The supernova remnant population of the Small Magellanic Cloud
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DOI：
10.1051/0004-6361/201936583
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发表时间：
2019-08
影响因子：
6.5
通讯作者：
P. Maggi;M. Filipović;B. Vukotić;J. Ballet;F. Haberl;C. Maitra;P. Kavanagh;M. Sasaki;M. Stupar
中科院分区：
文献类型：
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作者：
P. Maggi;M. Filipović;B. Vukotić;J. Ballet;F. Haberl;C. Maitra;P. Kavanagh;M. Sasaki;M. Stupar
目的：我们对小麦哲伦星云（SMC）的超新星遗迹（SNR）群体进行了全面的研究。我们测量了SMC信噪比的多波长特性，并将它们与大麦哲伦云（LMC）population.Methods进行了比较。本研究结合了SMC，档案和最近的无线电连续观测，光学线发射调查和新的光学光谱观测的大数据集ofXMM-牛顿观测。因此，我们能够建立一个完整和干净的样本19确认和4个候选SNR。均匀X射线光谱分析使我们能够搜索SN喷出物和铁K线发射，并测量星际介质丰度。我们估计的比率的核心崩溃，Ia型超新星率的SMC的基础上的X射线特性和当地的恒星环境的每个SNR.Results.After删除未经证实或错误分类的对象，并增加了两个新确认的SNRs的基础上多波长的功能，我们提出了一个最终的名单21确认的SNRs和两个候选人。虽然没有铁K线检测，即使是最明亮和最年轻的SNR，我们发现在11个SNR的SN喷出物的X射线证据。我们估计每颗超新星的核心坍缩超新星的分数为0.62-0.92（90%置信区间），高于LMC。这种差异可以归因于SMC中没有增强的恒星形成事件，这发生在LMC 0.5-1.5 Gyr前。O、Ne、Mg和Fe的热气体丰度是太阳的0.1-0.2倍。它们的比率，相对于SMC恒星丰度，反映了在SNR冲击的尘埃耗尽和部分尘埃破坏的影响。我们发现的证据表明，SMC信噪比探测的环境介质的平均扰动和密度较低，比在LMC，与两个星系的不同形态相一致。
Aims.We present a comprehensive study on the supernova remnant (SNR) population of the Small Magellanic Cloud (SMC). We measured multiwavelength properties of the SMC SNRs and compare them to those of the Large Magellanic Cloud (LMC) population.Methods.This study combines the large dataset ofXMM-Newtonobservations of the SMC, archival and recent radio continuum observations, an optical line emission survey, and new optical spectroscopic observations. We were therefore able to build a complete and clean sample of 19 confirmed and four candidate SNRs. The homogeneous X-ray spectral analysis allowed us to search for SN ejecta and Fe K line emission, and to measure interstellar medium abundances. We estimated the ratio of core-collapse to type Ia supernova rates of the SMC based on the X-ray properties and the local stellar environment of each SNR.Results.After the removal of unconfirmed or misclassified objects, and the addition of two newly confirmed SNRs based on multi-wavelength features, we present a final list of 21 confirmed SNRs and two candidates. While no Fe K line is detected even for the brightest and youngest SNR, we find X-ray evidence of SN ejecta in 11 SNRs. We estimate a fraction of 0.62–0.92 core-collapse supernova for every supernova (90% confidence interval), higher than in the LMC. The difference can be ascribed to the absence of the enhanced star-formation episode in the SMC, which occurred in the LMC 0.5–1.5 Gyr ago. The hot-gas abundances of O, Ne, Mg, and Fe are 0.1–0.2 times solar. Their ratios, with respect to SMC stellar abundances, reflect the effects of dust depletion and partial dust destruction in SNR shocks. We find evidence that the ambient medium probed by SMC SNRs is less disturbed and less dense on average than in the LMC, consistent with the different morphologies of the two galaxies.