Spectroscopic observations of progenitor activity 100 days before a Type Ibn supernova⋆,Astronomy & Astrophysics

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Spectroscopic observations of progenitor activity 100 days before a Type Ibn supernova⋆
Astronomy & Astrophysics ( IF 6.5 ) Pub Date : 2024-04-16 , DOI: 10.1051/0004-6361/202449350
S.J. Brennan , J. Sollerman , I. Irani , S. Schulze , P. Chen , K.K. Das , K. De , C. Fransson , A. Gal-Yam , A. Gkini , K.R. Hinds , R. Lunnan , D. Perley , Y.J. Qin , R. Stein , J. Wise ,

Obtaining spectroscopic observations of the progenitors of core-collapse supernovae is often unfeasible, due to an inherent lack of knowledge as to what stars experience supernovae and when they will explode. In this Letter we present photometric and spectroscopic observations of the progenitor activity of SN 2023fyq before the He-rich progenitor explodes as a Type Ibn supernova. The progenitor of SN 2023fyq shows an exponential rise in flux prior to core collapse. Complex He I emission line features are observed in the progenitor spectra, with a P Cygni-like profile, as well as an evolving broad base with velocities of the order of 10 000 km s^{−1^{. The luminosity and evolution of SN 2023fyq is consistent with a Type Ibn, reaching a peak r-band magnitude of −18.8 mag, although there is some uncertainty regarding the distance to the host, NGC 4388, which is located in the Virgo cluster. We present additional evidence of asymmetric He-rich material being present both prior to and after the explosion of SN 2023fyq, which suggests that this material survived the ejecta interaction. Broad [O I], C I, and the Ca II triplet lines are observed at late phases, confirming that SN 2023fyq was a genuine supernova, rather than a non-terminal interacting transient. SN 2023fyq provides insight into the final moments of a massive star’s life, demonstrating that the progenitor is likely highly unstable before core collapse.}}

中文翻译：

Ibn 型超新星爆发前 100 天的祖细胞活动的光谱观测⋆

由于固有地缺乏关于哪些恒星经历超新星以及它们何时爆炸的知识，获得核心塌陷超新星前身的光谱观测通常是不可行的。在这封信中，我们介绍了 SN 2023fyq 在富含 He 的前体爆炸为 Ibn 型超新星之前对 SN 2023fyq 前体活动的光度和光谱观测。 SN 2023fyq 的前身在核心崩溃之前显示出通量呈指数增长。在前体光谱中观察到复杂的 He I 发射线特征，具有类似 P Cygni 的轮廓，以及速度为 10 000 km s ^{-1数量级的不断演化的广泛基础^{。 SN 2023fyq 的光度和演化与 Ibn 型一致，达到了 -18.8 星等的峰值r波段星等，尽管与位于室女座星团的宿主 NGC 4388 的距离存在一些不确定性。我们提供了额外的证据，证明 SN 2023fyq 爆炸之前和之后都存在不对称富氦材料，这表明这种材料在喷射物相互作用中幸存下来。在后期观察到广泛的 [O I]、C I 和 Ca II 三重线，证实 SN 2023fyq 是一颗真正的超新星，而不是非末端相互作用瞬变。 SN 2023fyq 提供了对大质量恒星生命最后时刻的洞察，表明前身恒星在核心塌陷之前可能高度不稳定。}}

更新日期：2024-04-16

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PDF https://arxiv.org/pdf/2401.15148

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