The lowest-metallicity type II supernova from the highest-mass red supergiant progenitor-猫眼课题宝

DOI：

10.1038/s41550-018-0458-4

发表时间：

2018-05

期刊：

Nature Astronomy

影响因子：

14.1

通讯作者：

中科院分区：

物理与天体物理1区

文献类型：

作者：

J. Anderson;L. Dessart;C. Gutiérrez;T. Krühler;L. Galbany;A. Jerkstrand;S. Smartt;C. Contreras;N. Morrell;M. Phillips;M. Stritzinger;E. Hsiao;S. González-Gaitán;C. Agliozzo;C. Agliozzo;S. Castellón;K. Chambers;T. W. Chen;H. Flewelling;C. González;G. Hosseinzadeh;G. Hosseinzadeh;M. Huber;M. Fraser;C. Inserra;E. Kankare;S. Mattila;E. Magnier;K. Maguire;T. Lowe;J. Sollerman;M. Sullivan;D. Young;S. Valenti

红超巨星已被证实是大多数富氢II型超新星的祖星。然而，当这样的恒星被观测到质量为bbbb25 m⊙时（参考文献）。在美国，对bbbb18m⊙祖星的探测仍然难以捉摸。预计红超巨星也会以各种金属丰度形成，但发现的低金属丰度祖先的爆炸很少。在这里，我们报告了II型超新星SN 2015bs的观测结果，通过与光球相光谱模型的比较，我们推断其祖先金属丰度≤0.1Z⊙，通过与星云相光谱模型的比较，我们推断其零年龄主序质量为17-25M⊙。SN 2015bs显示出正常的“高原”光曲线形态和典型的光谱特性，暗示它是一颗红超巨星祖先。这是“正常”II型超新星的第一个高质量祖恒星，表明高质量红超巨星爆炸与低金属丰度祖恒星之间存在联系。

Red supergiants have been confirmed as the progenitor stars of the majority of hydrogen-rich type II supernovae. However, while such stars are observed with masses >25M⊙(ref. ), detections of >18M⊙progenitors remain elusive. Red supergiants are also expected to form at all metallicities, but discoveries of explosions from low-metallicity progenitors are scarce. Here, we report observations of the type II supernova, SN 2015bs, for which we infer a progenitor metallicity of ≤0.1Z⊙from comparison to photospheric-phase spectral models, and a zero-age main-sequence mass of 17–25M⊙through comparison to nebular-phase spectral models,. SN 2015bs displays a normal ‘plateau’ light-curve morphology, and typical spectral properties, implying a red supergiant progenitor. This is the first example of such a high-mass progenitor for a ‘normal’ type II supernova, suggesting a link between high-mass red supergiant explosions and low-metallicity progenitors.

The lowest-metallicity type II supernova from the highest-mass red supergiant progenitor

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