论文标题
II型超新星祖细胞的光度分布
Luminosity distribution of Type II supernova progenitors
论文作者
论文摘要
i介绍了112型II型超新星（SNE II）样本的祖细胞发光度（$ L $），直接根据祖细胞光度法和隆期校正技术计算，或者是从祖细胞亮度和[OI] $ 6300 $ 6364 LOISE $ 6364 LOINE $ nii plumin luminsusity的经验相关性的间接相关性，或者^550 $ niim uspes y ixplies usplosity plistos。自爆炸以来，在50 d时的绝对$ v $ - 带大小。为了校准这些相关性，我将十二个SNE II与祖细胞光度法测量的祖细胞发光性。我发现上面提到的相关性很强且具有统计学意义，并允许估计祖细胞亮度的精度20％至24％。我纠正了SN样本以进行选择偏置，并定义了一个112 SNE II的子样本，其祖细胞发光度之间具有$ \ log（l/l _ {\ odot}）= 4.6 $ dex，对应于校正样品的完整性限制，最大的近亲祖发亮度的完整性和$ \ log log（l/l/l/l/l/该子样本的光度分布在统计学上与LMC，SMC，M31和M33中的红色超级符号（RSG）的光度分布，$ 4.6 \ leq \ log（l/l _ {\ odot}）\ leq 5.091 $。这支持SN II祖细胞对应于RSG。与$ \ log（l/l _ {\ odot}）> 5.1 $ dex相对于RSG亮度分布（称为RSG问题）的显着缺失（l/l _ {\ odot}）> 5.1 $ dex在$ 5.2 \ pm0.5 \ f level中很重要。
I present progenitor luminosities ($L$) for a sample of 112 Type II supernovae (SNe II), computed directly from progenitor photometry and the bolometric correction technique, or indirectly from empirical correlations between progenitor luminosity and [OI] $λλ$6300, 6364 line luminosity at 350 d since explosion, $^{56}$Ni mass, or absolute $V$-band magnitude at 50 d since explosion. To calibrate these correlations, I use twelve SNe II with progenitor luminosities measured from progenitor photometry. I find that the correlations mentioned above are strong and statistically significant, and allow to estimate progenitor luminosities to a precision between 20 and 24 per cent. I correct the SN sample for selection bias and define a subsample of 112 SNe II with progenitor luminosities between $\log(L/L_{\odot})=4.6$ dex, corresponding to the completeness limit of the corrected sample, and the maximum observed progenitor luminosity of $\log(L/L_{\odot})=5.091$ dex. The luminosity distribution for this subsample is statistically consistent with those for red supergiants (RSGs) in LMC, SMC, M31, and M33 with $4.6\leq\log(L/L_{\odot})\leq5.091$. This supports that SN II progenitors correspond to RSGs. The conspicuous absence of SN II progenitors with $\log(L/L_{\odot})>5.1$ dex with respect to what is observed in RSG luminosity distributions, known as the RSG problem, is significant at a $5.2\pm0.5\,σ$ level.
