论文标题
103个剥离信封核心塌陷超新星的肾小球光谱的统计特性
Statistical properties of the nebular spectra of 103 stripped envelope core collapse supernovae
论文作者
论文摘要
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] 6300, 6363. The line profile and width of [O I] are employed to infer the ejecta geometry and the expansion velocity of the inner core.然后将这两个测量与SN子类型进行比较，然后将[O I]/[Ca II]比率进一步比较，该比率被用作祖细胞CO核心质量的指标。基于[O I]曲线的最佳拟合结果，将对象分类为不同的形态组，我们得出结论，与球形对称性的偏差是所有类型的sesne的共同特征。有一个暗示（约为1个sigma级别），在规范的sesne和Broad-Line SNE IC之间，线轮廓分数的分布不同。 [O I]宽度与[O I]/[Ca II]比率之间存在相关性，这表明富含氧气的材料倾向于更快地扩展具有更大的CO核心的物体。这种相关性可用于限制祖细胞质量与爆炸的动能之间的关系。此外，当[O I]/[Ca II]比率增加时，具有高斯[O I]曲线的物体的分数会增加，而具有双峰轮廓的对象则减小。这种现象连接了射流几何形状和祖细胞CO核心质量。
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] 6300, 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 sub types, 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 about 1 sigma 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] ratio 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] ratio 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.
