旋涡星系中核心坍缩超新星的径向分布
The radial distribution of core-collapse supernovae in spiral host galaxies
摘要：
与核心坍缩超新星的祖先的性质提供约束的目标，我们比较其螺旋宿主星系内的恒星和电离气体的分布在螺旋盘的径向分布。所有CCSNe的归一化径向分布符合指数规律，在等照度半径的五分之一内可能耗尽CCSNe。II型SNe分布的尺度长度似乎明显大于其宿主星系的恒星盘，但与弗里曼盘的尺度长度一致。SNe Ib/c的标度长度明显小于SNe II，Ib型和Ic型之间的差异很小。Ib/c型SNe的径向分布比弗里曼盘中的恒星更集中，但与我们推断的宿主星系的恒星盘分布相似。CCSN径向分布的尺度长度与宿主星系的形态类型或酒吧的存在没有显着的相关性。然而，低光度以及倾斜主机有一个不太集中的分布CCSNe，这可能是金属丰度和选择效应的结果，分别。CCSNe的指数分布显示了与电离气体一致的尺度长度，证实了普遍接受的假设，即这些SNe的祖先是年轻的大质量恒星。由于缺乏相关的CCSNe的归一化径向距离与宿主星系的形态类型，我们得出结论，更集中的分布SNe Ib/C相对于SNe II必须产生较高的金属丰度的祖先或可能从一个较浅的初始质量函数在内部区域的螺旋。
英文摘要：
With the goal of providing constraints on the nature of the progenitors of core-collapse supernovae, we compare their radial distribution within their spiral host galaxies with the distributions of stars and ionized gas in the spiral disks. The normalized radial distribution of all CCSNe is consistent with an exponential law, with a possible depletion of CCSNe within one-fifth of the isophotal radius. The scale length of the distribution of type II SNe appears to be significantly larger than that of the stellar disks of their host galaxies, but consistent with the scale lengths of Freeman disks. SNe Ib/c have a significantly smaller scale length than SNe II, with little difference between types Ib and Ic. The radial distribution of type Ib/c SNe is more centrally concentrated than that of the stars in a Freeman disk, but is similar to the stellar disk distribution that we infer for the host galaxies. The scale length of the CCSN radial distribution shows no significant correlation with the host galaxy morphological type, or the presence of bars. However, low luminosity as well as inclined hosts have a less concentrated distribution of CCSNe, which are probably a consequence of metallicity and selection effects, respectively. The exponential distribution of CCSNe shows a scale length consistent with that of the ionized gas confirming the generally accepted hypothesis that the progenitors of these SNe are young massive stars. Given the lack of correlation of the normalized radial distances of CCSNe with the morphological type of the host galaxy, we conclude that the more concentrated distribution of SNe Ib/c relative to SNe II must arise from the higher metallicity of their progenitors or possibly from a shallower initial mass function in the inner regions of spirals.
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