低光度型II SN\，2016 aqf：Ni/Fe丰度比的良好监测光谱演变
The low-luminosity type II SN\,2016aqf: A well-monitored spectral evolution of the Ni/Fe abundance ratio
摘要：
低光度II型超新星（LL SNe~II）是核塌缩超新星爆发能量较低的一端，但对它们的研究和物理认识还很有限。我们介绍了一个具有广泛光谱和光度覆盖的LL SN~II，SN 1，2016 aqf。我们测量了$V$ -带峰值的$-14.58$ \，mag，平台期的$\sim$ 100\，天，和推断的$^{56}$ Ni质量的$0.008 \pm 0.002$ \，\msun。峰值测辐射热光度L $_{\rm bol} \approx 10^{41.4}$、erg s $^{-1}$及其光谱演化是该类中其他SNe的典型特征。使用我们的后期光谱，我们测量[ \ion{O}{i} ] $λ\lambda6300, 6364$线，我们与SN II光谱合成模型进行比较，以限制祖先零年龄主序列质量。我们发现这是12 $\pm$ 3\，\msun。我们广泛的后期光谱覆盖的[ \ion{Fe}{ii} ] $\lambda7155$和[ \ion{Ni}{ii} ] $\lambda7378$线允许测量的Ni/Fe丰度比，一个参数敏感的内部祖结构和爆炸机制的动态。我们测量了$0.081^{+0.009}_{-0.010}$丰度比的一个恒定的演化，并认为测量丰度比的最佳时期是在爆炸后200 - 300天的$\sim$。我们把这个测量的背景下，SNE II的大样本和各种物理，光变曲线和光谱参数进行比较，在搜索的趋势，这可能允许间接的方式来约束这个比例。我们没有发现理论模型预测的相关性，然而，这可能是模型中参数和爆炸机制的精确选择，它们的简单性和/或测量的丰度比中的原始污染的结果。
英文摘要：
Low-luminosity type II supernovae (LL SNe~II) make up the low explosion energy end of core-collapse SNe, but their study and physical understanding remain limited. We present SN\,2016aqf, a LL SN~II with extensive spectral and photometric coverage. We measure a $V$-band peak magnitude of $-14.58$\,mag, a plateau duration of $\sim$100\,days, and an inferred $^{56}$Ni mass of $0.008 \pm 0.002$\,\msun. The peak bolometric luminosity, L$_{\rm bol} \approx 10^{41.4}$\,erg\,s$^{-1}$, and its spectral evolution is typical of other SNe in the class. Using our late-time spectra, we measure the [\ion{O}{i}] $λ\lambda6300, 6364$ lines, which we compare against SN II spectral synthesis models to constrain the progenitor zero-age main-sequence mass. We find this to be 12 $\pm$ 3\,\msun. Our extensive late-time spectral coverage of the [\ion{Fe}{ii}] $\lambda7155$ and [\ion{Ni}{ii}] $\lambda7378$ lines permits a measurement of the Ni/Fe abundance ratio, a parameter sensitive to the inner progenitor structure and explosion mechanism dynamics. We measure a constant abundance ratio evolution of $0.081^{+0.009}_{-0.010}$, and argue that the best epochs to measure the ratio are at $\sim$200 -- 300\,days after explosion. We place this measurement in the context of a large sample of SNe II and compare against various physical, light-curve and spectral parameters, in search of trends which might allow indirect ways of constraining this ratio. We do not find correlations predicted by theoretical models; however, this may be the result of the exact choice of parameters and explosion mechanism in the models, the simplicity of them and/or primordial contamination in the measured abundance ratio.
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