Circumstellar Interaction in the Ultraviolet Spectra of SN 2023ixf 14–66 Days After Explosion

K. Azalee Bostroem, David J. Sand, Luc Dessart, Nathan Smith, Saurabh W. Jha, Stefano Valenti, Jennifer E. Andrews, Yize Dong, 一泽 董, Alexei V. Filippenko, Sebastian Gomez, Daichi Hiramatsu, Emily T. Hoang, Griffin Hosseinzadeh, D. Andrew Howell, Jacob E. Jencson, Michael Lundquist, Curtis McCully, Darshana Mehta, Nicolas E. Meza-Retamal, Jeniveve Pearson, Aravind P. Ravi, Manisha Shrestha and Samuel Wyatt
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Abstract

SN 2023ixf was discovered in M101 within a day of the explosion and rapidly classified as a Type II supernova with flash features. Here we present ultraviolet (UV) spectra obtained with the Hubble Space Telescope 14, 19, 24, and 66 days after the explosion. Interaction between the supernova ejecta and circumstellar material (CSM) is seen in the UV throughout our observations in the flux of the first three epochs and asymmetric Mg ii emission on day 66. We compare our observations to CMFGEN supernova models that include CSM interaction ( M⊙ yr−1) and find that the power from CSM interaction is decreasing with time, from Lsh ≈ 5 × 1042 erg s−1 to Lsh ≈ 1 × 1040 erg s−1 between days 14 and 66. We examine the contribution of individual atomic species to the spectra on days 14 and 19, showing that the majority of the features are dominated by iron, nickel, magnesium, and chromium absorption in the ejecta. The UV spectral energy distribution of SN 2023ixf sits between that of supernovae, which show no definitive signs of CSM interaction, and those with persistent signatures assuming the same progenitor radius and metallicity. Finally, we show that the evolution and asymmetric shape of the Mg iiλλ 2796, 2802 emission are not unique to SN 2023ixf. These observations add to the early measurements of dense, confined CSM interaction, tracing the mass-loss history of SN 2023ixf to ∼33 yr prior to the explosion and the density profile to a radius of ∼5.7 × 1015 cm. They show the relatively short evolution from a quiescent red supergiant wind to high mass loss.
SN 2023ixf 爆炸后 14-66 天紫外光谱中的环星相互作用
SN 2023ixf 在爆炸后一天内在 M101 中被发现,并迅速被归类为具有闪光特征的 II 型超新星。在这里,我们展示了用哈勃太空望远镜获得的爆炸后14、19、24和66天的紫外线(UV)光谱。在整个紫外观测过程中,我们看到了超新星喷出物与星周物质(CSM)之间的相互作用,前三个时间段的通量和第66天的不对称Mg ii发射。我们将观测结果与包含CSM相互作用(M⊙ yr-1)的CMFGEN超新星模型进行了比较,发现CSM相互作用的功率随着时间的推移而减小,在第14天到第66天之间,从Lsh ≈ 5 × 1042 erg s-1减小到Lsh ≈ 1 × 1040 erg s-1。我们研究了第14天和第19天的光谱中各个原子种类的贡献,结果表明大部分特征都是由喷出物中的铁、镍、镁和铬的吸收所主导的。SN 2023ixf 的紫外光谱能量分布介于超新星和具有持续特征的超新星之间,前者没有显示出 CSM 相互作用的明确迹象,而后者则假定原生半径和金属度相同。最后,我们证明了Mg iiλλ 2796,2802发射的演变和不对称形状并不是SN 2023ixf所独有的。这些观测增加了对致密、封闭的CSM相互作用的早期测量,追溯了SN 2023ixf的质量损失历史至爆炸前33年,密度剖面至半径5.7 × 1015厘米。它们显示了从静态红超巨星风到高质量损失的相对较短的演化过程。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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