Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve
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DOI：
10.3847/2041-8213/acb0d0
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发表时间：
2022-11
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通讯作者：
Qinan Wang;P. Armstrong;Y. Zenati;R. Ridden-Harper;A. Rest;I. Arcavi;C. Kilpatrick;R. Foley;B. Tucker;C. Lidman;T. Killestein;M. Shahbandeh;Joseph P. Anderson;R. Angulo;C. Ashall;J. Burke;Ting-Wan Chen;Sophie von Coelln;Kyle A. Dalrymple;K. W. Davis;M. Fulton;L. Galbany;E. P. Gonzalez;Bore Gao;M. Gromadzki;D. Howell;N. Ihanec;J. Jencson;David O. Jones;J. Lyman;C. McCully;T. Müller-Bravo;M. Newsome;M. Nicholl;D. O’Neill;C. Pellegrino;S. Rest;S. Smartt;Kenneth W. Smith;S. Srivastav;G. Terreran;S. Tinyanont;D. Young;A. Zenteno
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作者：
Qinan Wang;P. Armstrong;Y. Zenati;R. Ridden-Harper;A. Rest;I. Arcavi;C. Kilpatrick;R. Foley;B. Tucker;C. Lidman;T. Killestein;M. Shahbandeh;Joseph P. Anderson;R. Angulo;C. Ashall;J. Burke;Ting-Wan Chen;Sophie von Coelln;Kyle A. Dalrymple;K. W. Davis;M. Fulton;L. Galbany;E. P. Gonzalez;Bore Gao;M. Gromadzki;D. Howell;N. Ihanec;J. Jencson;David O. Jones;J. Lyman;C. McCully;T. Müller-Bravo;M. Newsome;M. Nicholl;D. O’Neill;C. Pellegrino;S. Rest;S. Smartt;Kenneth W. Smith;S. Srivastav;G. Terreran;S. Tinyanont;D. Young;A. Zenteno
我们对双峰型超新星(SNIIb)SN2021zby进行了早期观测和分析。TESS在爆炸后10天的第一个∼内以30分钟的节奏捕捉到了SN2021zby的显著早期激波冷却峰值。我们给出了SN2021zby的光学和近红外光谱系列，包括激波冷却阶段的三个光谱。通过多带模型拟合，我们发现它的前身与红色超巨星或黄色超巨星的性质是一致的，包络质量为∼0.30-0.65M⊙，包络半径为∼120-300R⊙。这些推断的祖细胞特性与其他具有双峰特征的SNE IIb相似，如SNE 1993j、2011dh、2016gkg和2017jgh。这项研究进一步验证了高频率和早期覆盖在解决激波-冷却光曲线形状方面的重要性，同时多波段观测，特别是紫外线，也是完全限制前驱特性所必需的。
We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS captured the prominent early shock-cooling peak of SN 2021zby within the first ∼10 days after explosion with a 30 minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock-cooling phase. Using a multiband model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of ∼0.30–0.65 M ⊙ and an envelope radius of ∼120–300 R ⊙. These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked feature, such as SNe 1993J, 2011dh, 2016gkg, and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock-cooling light curve, while the multiband observations, particularly UV, are also necessary to fully constrain the progenitor properties.