Statistical Properties of the Nebular Spectra of 103 Stripped-envelope Core-collapse Supernovae
Statistical Properties of the Nebular Spectra of 103 Stripped-envelope Core-collapse Supernovae
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DOI：
10.3847/1538-4357/ac4f60
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发表时间：
2022-01
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影响因子：
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通讯作者：
Qiliang 其亮 Fang 方;K. Maeda;H. Kuncarayakti;Masaomi Tanaka;K. Kawabata;T. Hattori;K. Aoki;T. Moriya;M. Yamanaka
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作者：
Qiliang 其亮 Fang 方;K. Maeda;H. Kuncarayakti;Masaomi Tanaka;K. Kawabata;T. Hattori;K. Aoki;T. Moriya;M. Yamanaka
我们分析了从2002年到2012年用斯巴鲁望远镜观测到的103颗剥离包络超新星的星云光谱，重点是[O I]λλ6300,6363。[O I]的线型和宽度被用来推断喷出的几何形状和内核的膨胀速度，然后将这两个测量值与SN亚型进行比较，并进一步与[O I]/[Ca II]比值进行比较，[O I]/[Ca II]比值被用作前驱CO核质量的指示器。根据[O I]轮廓的最佳拟合结果，将目标划分为不同的形态群，并得出结论：偏离球对称是所有类型的SESNe的共同特征。有一个线索(在∼1σ水平上)，线轮廓分数的分布在标准SSNE和宽线SINE IC之间是不同的。发现了[O I]宽度和[O I]/[Ca II]之间的关系，这表明对于具有更大质量的CO核的物体，富氧物质往往膨胀得更快。这种关联性可以用来限制前驱物质质量和爆炸动能之间的关系。此外，随着[O I]/[Ca II]的增加，具有高斯[O I]轮廓的物体比例增加，而具有双峰轮廓的物体比例减少。这一现象将抛射几何形状和前驱CO核心质量联系在一起。
We present an analysis of the nebular spectra of 103 stripped-envelope (SE) supernovae (SNe) collected from the literature and observed with the Subaru Telescope from 2002 to 2012, focusing on [O i] λλ6300, 6363. The line profile and width of [O i] are employed to infer the ejecta geometry and the expansion velocity of the inner core; these two measurements are then compared with the SN subtypes, and further with the [O i]/[Ca ii] ratio, which is used as an indicator of the progenitor CO core mass. Based on the best-fit results of the [O i] profile, the objects are classified into different morphological groups, and we conclude that the deviation from spherical symmetry is a common feature for all types of SESNe. There is a hint (at the ∼1σ level) that the distributions of the line profile fractions are different between canonical SESNe and broad-line SNe Ic. A correlation between [O i] width and [O i]/[Ca ii] is discerned, indicating that the oxygen-rich material tends to expand faster for objects with a more massive CO core. Such a correlation can be utilized to constrain the relation between the progenitor mass and the kinetic energy of the explosion. Further, when [O i]/[Ca ii] increases, the fraction of objects with Gaussian [O i] profile increases, while those with double-peaked profile decreases. This phenomenon connects ejecta geometry and the progenitor CO core mass.