A statistical study of the environmental age of core-collapse supernovae based on VLT/MUSE integral-field-unit spectroscopy
University of Chinese Academy of Sciences（中国科学院大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；National and Kapodistrian University of Athens（雅典国立卡波迪斯特里阿斯大学）；Foundation for Research and Technology-Hellas（希腊研究与技术基金会）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）
Qiang Xi, Ning-Chen Sun, Yihan Zhao, Emmanouil Zapartas, Dimitris Souropanis, Chun Chen, Xiaohan Chen, César Rojas-Bravo, Justyn R. Maund, Zexi Niu, Adam J. Sin… 展开作者
Qiang Xi, Ning-Chen Sun, Yihan Zhao, Emmanouil Zapartas, Dimitris Souropanis, Chun Chen, Xiaohan Chen, César Rojas-Bravo, Justyn R. Maund, Zexi Niu, Adam J. Singleton, Anyu Wang, Zhiyi Wang, Ziyang Wang, Junjie Wu, Jifeng Liu
We aim to understand the progenitor channels of CCSNe via a statistical study of the ages of their environments. We compiled a large and minimally biased sample of 128 CCSNe discovered by untargeted wide-field transient surveys and with archival VLT/MUSE integral-field-unit spectroscopy. We measured the local Hα luminosity within a 300-pc aperture centered on the SN explosion site as an empirical proxy for the environmental age. We find that the mean local H$α$ luminosities are ordered as II(P) $\approx$ IIb $\lesssim$ Ib $<$ Ic. The differences among Types~II(P), IIb and Ib are very small, if any. Type~Ic SNe are located in clearly younger environments than the other types. Our result suggests that Type Ic SNe have much younger and more massive progenitors than the other CCSN types and they likely originate from a distinct progenitor channel. The distinction between Types II(P), IIb and Ib SNe is insensitive to progenitor mass and mainly due to the different binary separation; in contrast, Type Ic SNe predominantly require much higher-mass progenitors accompanied by close companions with large mass ratios and/or much stronger stellar wind that depends sensitively on progenitor mass.
A characterization of ASAS-SN core-collapse supernova environments with VLT+MUSE: I. Sample selection, analysis of local environments, and correlations with light curve properties
研究基于 ASAS-SN 均匀样本与 VLT/MUSE 观测，分析112颗核心坍缩超新星的局地 HII 区环境，揭示不同类型环境差异及光变曲线参数与 SFR、Hα EW 和氧丰度的关联。
Characterizing the Low-Mass Pre-Main-Sequence Population in the Low-Metallicity Star-Forming Region Dolidze 25 Using VLT-MUSE
Indian Institute of Science Education and Research Tirupati（印度科学教育与研究学院提鲁帕蒂分校）；Peking University（北京大学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Rice University（莱斯大学）；University of Cumbria（坎布里亚大学）
MUSE Integral Field Observations of the Oxygen-rich SNR 1E 0102.2-7219
我们在赛丁泉天文台用积分场光谱仪WiFeS对富氧SNR 1 E 0102.2-7219进行了观测，首次发现了富硫喷出物。后续的深DDT观测与MUSE对VLT（源上的8100 s）导致了快速移动的氢以及富氩和富氯物质的额外发现。快速移动的氢结的探测挑战了1 E 0102的祖先是沃尔夫-拉叶星的致密核心的解释，该恒星已经摆脱了整个外壳。除了探测到氢和氧燃烧的产物之外，这张前所未有的清晰（0.2”的光谱尺寸，约0.7”的视宁度）和麦哲伦云中富含氧的SNR的深MUSE视图揭示了进一步令人兴奋的发现，包括[Fe xiv]λ5303和[Fe xi]λ7892发射，我们将其与前向冲击波联系起来。我们提出了这个令人兴奋的数据集，并讨论了它的爆炸机制和相关的超新星核合成的一些影响。
Linear spectropolarimetry of 35 Type Ia Supernovae with VLT/FORS: An analysis of the Si II line polarization
光谱偏振使我们能够测量超新星爆炸中喷出物的几何形状和化学结构，这对于理解其爆炸机制和祖先系统至关重要。我们收集了35个Ia型超新星（SNe Ia）的档案数据，用甚大望远镜上的FORS观测，共127个历元。我们研究了Si II $λ$ 6355 $Å$线（p $_{\rm Si II}$）的偏振作为时间的函数，可以看出其在相对于最大亮度的各种偏振度和时期的范围内达到峰值。我们再现了在以前的研究中确定的$Δ$ m $_{15}$ -p $_{\rm Si II}$关系，并表明亚发光和过渡物体显示的偏振值低于正常Ia型超新星的$Δ$ m $_{15}$ -p $_{\rm Si II}$关系。我们发现了一个统计上显着的线性关系的Si II $λ$ 6355 $Å$线的偏振之前的最大亮度和Si II线速度，并建议这一点，随着$Δ$ m $_{15}$ -P $_{\rm Si II}$的关系，可以解释的延迟爆炸模型的上下文中。相比之下，我们比较了我们的观察$Δ$ m $_{15}$ -v $_{\rm Si II}$平面中的数值预测，并发现了一个二分法之间的极化性质的Bracrasekhar和sub-Bracrasekhar质量爆炸，这支持了两种不同的爆炸机制的可能性。SNe的子样本显示在$q$ - $u$平面中的环的演化，这表明具有深度的更复杂的Si结构。这种见解，这不能收集到的总通量谱…
