核心坍缩超新星与年轻和年老恒星星族径向分布的比较
Comparisons of the radial distributions of core-collapse supernovae with those of young and old stellar populations
摘要：
我们提出的观测约束的性质的核心坍缩超新星通过调查其径向分布相对于年轻和年老的恒星星族在其宿主星系，跟踪的H-α发射和R-波段光。我们讨论的结果和它们对超新星祖先的性质的影响，为样本的177核心坍缩超新星。我们发现，整个核心坍缩人口的径向位置密切遵循的径向分布的H-α发射，这意味着两者都是很好的示踪剂的恒星形成的星系内。在这个总体分布中，我们发现有一个SNII的中心赤字，它被SNIb/c的中心过剩所抵消。这意味着强烈的金属丰度依赖于两种类型的相对产量，SNIb/c产生于比SNII更高的金属丰度祖先。将SNIb/c分成单独的类别，我们发现，在从SNII到SNIb到SNIc的祖金属丰度方面出现了一种趋势，后者来自最高金属丰度的祖金属丰度。
英文摘要：
We present observational constraints on the nature of core-collapse supernovae through an investigation into their radial distributions with respect to those of young and old stellar populations within their host galaxies, as traced by H-alpha emission and R-band light respectively. We discuss results and the implications they have on the nature of supernova progenitors, for a sample of 177 core-collapse supernovae. We find that the radial positions of the overall core-collapse population closely follow the radial distribution of H-alpha emission, implying that both are excellent tracers of star formation within galaxies. Within this overall distribution we find that there is a central deficit of SNII which is offset by a central excess of SNIb/c. This implies a strong metallicity dependence on the relative production of the two types, with SNIb/c arising from higher metallicity progenitors than SNII. Separating the SNIb/c into individual classes we find that a trend emerges in terms of progenitor metallicity going from SNII through SNIb to SNIc, with the latter arising from the highest metallicity progenitors.
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