LONG-DURATION SUPERLUMINOUS SUPERNOVAE AT LATE TIMES
LONG-DURATION SUPERLUMINOUS SUPERNOVAE AT LATE TIMES
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DOI：
10.3847/1538-4357/835/1/13
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发表时间：
2016-08
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通讯作者：
A. Jerkstrand;S. Smartt;C. Inserra;M. Nicholl;T. W. Chen;T. Krühler;J. Sollerman;S. Taubenberger;A. Gal-yam;E. Kankare;K. Maguire;M. Fraser;S. Valenti;M. Sullivan;R. Cartier;D. Young
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作者：
A. Jerkstrand;S. Smartt;C. Inserra;M. Nicholl;T. W. Chen;T. Krühler;J. Sollerman;S. Taubenberger;A. Gal-yam;E. Kankare;K. Maguire;M. Fraser;S. Valenti;M. Sullivan;R. Cartier;D. Young
本文介绍了Ic型超亮超新星（SLSNe）的星云相观测和光谱模型。LSQ 14 an和SN 2015 bn都显示出与SN 2007 bi类似的晚期光谱，并且这类光谱与SN 1998 bw等宽线SNe Ic有很强的相似性。SN 2015 bn的近红外观测显示出很强的Ca ii三重态，O i 9263，O i 1.13 μm，Mg i 1.50 μm，但没有明显的He，Si或S发射。高Ca ii NIR/[Ca ii] 7291，7323比值为1.02，表明高电子密度为cm−3。研究了氧区发射的光谱模型，对发射区进行了约束。模型需要M来产生足够的[O i] 6300，6364光度，而不考虑供电情况和密度。高氧区质量，由高估计镁质量支持，指向大规模CO核心的爆炸，需要。对不稳定脉动的碰撞不能提供足够的质量来解释发射。[O ii]和[O iii]线在许多模型中自然出现，这加强了在某些光谱中对宽[O ii] 7320，7330，[O iii] 4363和[O iii] 4959，5007的识别。在Mg i] 4571、Mg i 1.504 μm和O i复合谱线上，O/Mg区需要一个小的填充因子才能产生足够的亮度，这表明喷出物是成团的。我们审查的背景下提出的SLSNe的各种方案的星云光谱建模的约束。
Nebular-phase observations and spectral models of Type Ic superluminous supernovae (SLSNe) are presented. LSQ14an and SN 2015bn both display late-time spectra similar to galaxy-subtracted spectra of SN 2007bi, and the class shows strong similarity with broad-lined SNe Ic such as SN 1998bw. Near-infrared observations of SN 2015bn show a strong Ca ii triplet, O i 9263, O i 1.13 μm, and Mg i 1.50 μm, but no distinct He, Si, or S emission. The high Ca ii NIR/[Ca ii] 7291, 7323 ratio of ∼2 indicates a high electron density of cm−3. Spectral models of oxygen-zone emission are investigated to put constraints on the emitting region. Models require M⊙ to produce enough [O i] 6300, 6364 luminosity, irrespective of the powering situation and the density. The high oxygen-zone mass, supported by high estimated magnesium masses, points to explosions of massive CO cores, requiring . Collisions of pair-instability pulsations do not provide enough mass to account for the emission. [O ii] and [O iii] lines emerge naturally in many models, which strengthens the identification of broad [O ii] 7320, 7330, [O iii] 4363, and [O iii] 4959, 5007 in some spectra. A small filling factor for the O/Mg zone is needed to produce enough luminosity in Mg i] 4571, Mg i 1.504 μm, and O i recombination lines, which shows that the ejecta is clumped. We review the constraints from the nebular spectral modeling in the context of the various scenarios proposed for SLSNe.