Broad-lined Supernova 2016coi with a Helium Envelope
Broad-lined Supernova 2016coi with a Helium Envelope
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DOI：
10.3847/1538-4357/aa5f57
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发表时间：
2017-02
期刊：
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通讯作者：
M. Yamanaka;T. Nakaoka;Masaomi Tanaka;K. Maeda;S. Honda;H. Hanayama;T. Morokuma;M. Imai;K. Kinugasa;K. Murata;T. Nishimori;O. Hashimoto;Hirotaka Gima;K. Hosoya;Ayano Ito;M. Karita;M. Kawabata;K. Morihana;Yuto Morikawa;K. Murakami;T. Nagayama;Tatsuharu Ono;H. Onozato;Y. Sarugaku;M. Sato;D. Suzuki;J. Takahashi;M. Takayama;Hijiri Yaguchi;H. Akitaya;Y. Asakura;K. Kawabata;D. Kuroda;D. Nogami;Y. Oasa;T. Omodaká;Y. Saito;K. Sekiguchi;N. Tominaga;M. Uemura;Makoto Watanabe
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文献类型：
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作者：
M. Yamanaka;T. Nakaoka;Masaomi Tanaka;K. Maeda;S. Honda;H. Hanayama;T. Morokuma;M. Imai;K. Kinugasa;K. Murata;T. Nishimori;O. Hashimoto;Hirotaka Gima;K. Hosoya;Ayano Ito;M. Karita;M. Kawabata;K. Morihana;Yuto Morikawa;K. Murakami;T. Nagayama;Tatsuharu Ono;H. Onozato;Y. Sarugaku;M. Sato;D. Suzuki;J. Takahashi;M. Takayama;Hijiri Yaguchi;H. Akitaya;Y. Asakura;K. Kawabata;D. Kuroda;D. Nogami;Y. Oasa;T. Omodaká;Y. Saito;K. Sekiguchi;N. Tominaga;M. Uemura;Makoto Watanabe
我们给出了宽线（BL）超新星（SN） 2016coi在估计爆炸日期后t = 7至67天的早期光谱和光曲线。该SN最初被报道为BL型SN - Ic （SN Ic-BL）。然而，我们发现在t = 12天以内的光谱呈现出λ5876， λ6678和λ7065的吸收谱线。我们发现，正常snib的平滑和蓝移光谱与SN 2016coi的观测光谱非常相似。SN 2016coi的线速度与SNe Ic-BL相似，且明显快于SNe Ib，线速度和光曲线分析表明，SN 2016coi的动能和总喷射质量与SNe Ic-BL相似。与已报道发现He i的BL SNe 2009bb和2012ap一起，这些SNe可能是SNe Ic-BL和SNe Ib之间的过渡天体，可归类为BL型“Ib”SNe （SNe“Ib”-BL）。我们的研究表明，bsne最外层的多样性可能与进化路径的多样性有关。
We present the early-phase spectra and the light curves of the broad-lined (BL) supernova (SN) 2016coi from t = 7 to 67 days after the estimated explosion date. This SN was initially reported as a BL Type SN Ic (SN Ic-BL). However, we found that spectra up to t = 12 days exhibited the He i λ5876, λ6678, and λ7065 absorption lines. We show that the smoothed and blueshifted spectra of normal SNe Ib are remarkably similar to the observed spectrum of SN 2016coi. The line velocities of SN 2016coi were similar to those of SNe Ic-BL and significantly faster than those of SNe Ib. Analyses of the line velocity and light curve suggest that the kinetic energy and the total ejecta mass of SN 2016coi are similar to those of SNe Ic-BL. Together with BL SNe 2009bb and 2012ap, for which the detection of He i was also reported, these SNe could be transitional objects between SNe Ic-BL and SNe Ib, and be classified as BL Type “Ib” SNe (SNe “Ib”-BL). Our work demonstrates the diversity of the outermost layer in BL SNe, which should be related to the variety of the evolutionary paths.