SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
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DOI：
10.3847/2041-8213/acf2ec
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发表时间：
2023-06
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通讯作者：
W. Jacobson-Galán;L. Dessart;R. Margutti;R. Chornock;R. Foley;C. Kilpatrick;D. Jones;Kirsty Taggart;C. Angus;S. Bhattacharjee;L. A. Braff;D. Brethauer;A. Burgasser;F. Cao;C. Carlile;K. Chambers;D. Coulter;E. Dominguez-Ruiz;C. Dickinson;T. D. Boer;Alexander T Gagliano;C. Gall;H. Gao;E. Gates;S. Gomez;M. Guolo;M. Halford;J. Hjorth;M. Huber;M. N. Johnson;P. Karpoor;T. Laskar;N. LeBaron;Z. Li;Y. Lin;S. Loch;P. Lynam;E. Magnier;P. Maloney;D. Matthews;M. McDonald;Hong-Yan Miao;D. Milisavljevic;Y.-C. Pan;S. Pradyumna;C. Ransome;J. Rees;A. Rest;C. Rojas-Bravo;N. Sandford;L. Ascencio;S. Sanjaripour;A. Savino;H. Sears;N. Sharei;S. Smartt;E. Softich;C. Theissen;S. Tinyanont;H. Tohfa;V. Villar;Q. Wang;R. Wainscoat;A. Westerling;E. Wiston;M. Wozniak;S. Yadavalli;Y. Zenati
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作者：
W. Jacobson-Galán;L. Dessart;R. Margutti;R. Chornock;R. Foley;C. Kilpatrick;D. Jones;Kirsty Taggart;C. Angus;S. Bhattacharjee;L. A. Braff;D. Brethauer;A. Burgasser;F. Cao;C. Carlile;K. Chambers;D. Coulter;E. Dominguez-Ruiz;C. Dickinson;T. D. Boer;Alexander T Gagliano;C. Gall;H. Gao;E. Gates;S. Gomez;M. Guolo;M. Halford;J. Hjorth;M. Huber;M. N. Johnson;P. Karpoor;T. Laskar;N. LeBaron;Z. Li;Y. Lin;S. Loch;P. Lynam;E. Magnier;P. Maloney;D. Matthews;M. McDonald;Hong-Yan Miao;D. Milisavljevic;Y.-C. Pan;S. Pradyumna;C. Ransome;J. Rees;A. Rest;C. Rojas-Bravo;N. Sandford;L. Ascencio;S. Sanjaripour;A. Savino;H. Sears;N. Sharei;S. Smartt;E. Softich;C. Theissen;S. Tinyanont;H. Tohfa;V. Villar;Q. Wang;R. Wainscoat;A. Westerling;E. Wiston;M. Wozniak;S. Yadavalli;Y. Zenati
我们展示了 SN 2023ixf 的紫外和/或光学观测结果和模型，SN 2023ixf 是一颗位于 Messier 101 的 II 型超新星 (SN)，速度为 6.9 Mpc。 SN 2023ixf 的早期（闪光）光谱主要在利克天文台获得，揭示了 H i、He i/ii、C iv 和 N iii/iv/v 的发射线，具有狭窄的核心和宽阔、对称的翼，这些发射线是由于激波爆发之前位于祖星周围的致密、近距离星周材料 (CSM) 的光电离而产生的。这些电子散射加宽的线轮廓相对于第一束光持续约 8 天，此时多普勒加宽了最快的 SN 喷射物形式的特征，表明在 r ≳ 1015 cm 时 CSM 密度降低。 SN 2023ixf 的早期光变曲线显示峰值绝对星等（例如，M u = -18.6 mag，M g = -18.4 mag），比典型的 II 型 SNe 亮≳2 mag，这种光度增强也与 CSM 相互作用提供的冲击功率一致。将 SN 2023ixf 与来自非 LTE 辐射传输代码 CMFGEN 和辐射流体动力学代码 HERACLES 的光曲线和多历元光谱模型的网格进行比较表明，密集的太阳金属丰度 CSM 仅限于 r = (0.5–1) × 1015 cm，并且前体质量损失率为 Ṁ=10−2M⊙ yr−1。对于假设的原始风速 v w = 50 km s−1，这对应于爆炸前最后 3-6 年期间质量损失的增强（即超级风阶段）。
We present UV and/or optical observations and models of SN 2023ixf, a type II supernova (SN) located in Messier 101 at 6.9 Mpc. Early time (flash) spectroscopy of SN 2023ixf, obtained primarily at Lick Observatory, reveals emission lines of H i, He i/ii, C iv, and N iii/iv/v with a narrow core and broad, symmetric wings arising from the photoionization of dense, close-in circumstellar material (CSM) located around the progenitor star prior to shock breakout. These electron-scattering broadened line profiles persist for ∼8 days with respect to first light, at which time Doppler broadened the features from the fastest SN ejecta form, suggesting a reduction in CSM density at r ≳ 1015 cm. The early time light curve of SN 2023ixf shows peak absolute magnitudes (e.g., M u = −18.6 mag, M g = −18.4 mag) that are ≳2 mag brighter than typical type II SNe, this photometric boost also being consistent with the shock power supplied from CSM interaction. Comparison of SN 2023ixf to a grid of light-curve and multiepoch spectral models from the non-LTE radiative transfer code CMFGEN and the radiation-hydrodynamics code HERACLES suggests dense, solar-metallicity CSM confined to r = (0.5–1) × 1015 cm, and a progenitor mass-loss rate of Ṁ=10−2M⊙ yr−1. For the assumed progenitor wind velocity of v w = 50 km s−1, this corresponds to enhanced mass loss (i.e., superwind phase) during the last ∼3–6 yr before explosion.