论文标题
II-P型超新星2019mhm和祖细胞系统的约束
The Type II-P Supernova 2019mhm and Constraints on Its Progenitor System
论文作者
论文摘要
我们介绍了位于NGC〜6753的II-P型超新星（SN〜II-P）2019MHM的爆炸前和探索后观察结果。基于光谱和光度法，我们表明SN \，2019MHM表现出较宽的氢线，其速度为$ -8500 \ pm200 $ 〜km〜s $ s $^{ - 1} $和$ 111 \ pm2 $ 〜pm2 $ 〜Day Day Extended exted extded exted exted exted exted parted parted parted parted parted parted parted plated in type-ii-p suplass type type ii-pecplass典型。我们还适合其延迟降压光曲线，并推断它最初产生了$ 1.3 \ times 10^{ - 2} $ 〜M $ _ {\ odot} \ odot} \ pm 5.5 \ pm 5.5 \ pm 5.5 \ times 10^{ - 4} $〜$ m_ \ m_ \ odot $。在爆炸前19年获得的{\ it Hubble Space望远镜}上的宽阔田野行星相机2的成像，我们与示例后的宽场摄像机3图像保持一致，并证明SN与SN相当于$> $> $> $> $> $> $> $> $> $> $> $> $> $> $ 24.53〜mag，f814w for a f 814w for $> agement for $> 4 <-7.7 $ 〜MAG。与大型明星进化轨道相比，我们确定祖细胞星有最大零老年主序列质量$ <$ <$ 17.5〜m $ _ {\ odot} $，与其他SN〜II-P祖细胞一致。 SN \，2019MHM可以添加到不断增长的SNE〜II-P人群中，对其祖细胞恒星的亮度和良好的SN特性都有直接限制。
We present pre- and post-explosion observations of the Type II-P supernova (SN~II-P) 2019mhm located in NGC~6753. Based on optical spectroscopy and photometry, we show that SN\,2019mhm exhibits broad lines of hydrogen with a velocity of $-8500\pm200$~km~s$^{-1}$ and a $111\pm2$~day extended plateau in its luminosity, typical of the Type II-P subclass. We also fit its late-time bolometric light curve and infer that it initially produced a ${}^{56}$Ni mass of $1.3 \times 10^{-2}$~M$_{\odot} \pm 5.5 \times 10^{-4}$~$M_\odot$. Using imaging from the Wide Field Planetary Camera 2 on the {\it Hubble Space Telescope} obtained 19~years before explosion, we aligned to a post-explosion Wide Field Camera 3 image and demonstrate that there is no detected counterpart to the SN to a limit of $>$24.53~mag in F814W, corresponding to an absolute magnitude limit of $M_{\rm F814W} < -7.7$~mag. Comparing to massive-star evolutionary tracks, we determine that the progenitor star had a maximum zero-age main sequence mass $<$17.5~M$_{\odot}$, consistent with other SN~II-P progenitor stars. SN\,2019mhm can be added to the growing population of SNe~II-P with both direct constraints on the brightness of their progenitor stars and well-observed SN properties.
