SN 2010kd: Photometric and Spectroscopic Analysis of a Slow-decaying Superluminous Supernova
SN 2010kd: Photometric and Spectroscopic Analysis of a Slow-decaying Superluminous Supernova
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DOI：
10.3847/1538-4357/ab737b
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发表时间：
2020-02
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通讯作者：
Amit Kumar;S. Pandey;R. Konyves-Toth;R. Staten;J. Vinkó;J. Wheeler;Wei Zheng;A. Filippenko;R. Kehoe;R. Quimby;Yuan Fang;C. Akerlof;T. Mckay;E. Chatzopoulos;B. Thomas;G. Dhungana;A. Aryan;R. Dastidar;A. Gangopadhyay;Rahul Gupta;K. Misra;B. Kumar;N. Brahme;D. Buckley
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作者：
Amit Kumar;S. Pandey;R. Konyves-Toth;R. Staten;J. Vinkó;J. Wheeler;Wei Zheng;A. Filippenko;R. Kehoe;R. Quimby;Yuan Fang;C. Akerlof;T. Mckay;E. Chatzopoulos;B. Thomas;G. Dhungana;A. Aryan;R. Dastidar;A. Gangopadhyay;Rahul Gupta;K. Misra;B. Kumar;N. Brahme;D. Buckley
本文介绍了SN 2010 kd的数据和分析，这是一颗低红移（z = 0.101）的缺氢超亮超新星（SLSN），基于紫外/光学光度学和光谱学，相对于B波段最大光，跨度为−28至+194天。SN 2010 kd的B波段光变曲线与一个已被充分研究的SLSNe I的子集在红移相当的情况下的比较表明，它是一个缓慢衰变的PTF 12坝状SLSN。使用Minim代码进行的分析光变曲线建模表明，SN 2010 kd的热光变曲线有利于星周物质相互作用的动力机制。SYNAPPS建模的早期阶段的光谱不确定广泛的H或He线，而光球相光谱主要由O i，O ii，C ii，C iv，和Si ii，特别是存在的低和高速度组件的O ii和Si ii线。SN 2010 kd的星云相谱主要由O i和Ca ii发射线组成，与其他SLSNe I相似。SN 2010 kd的线速度演化曲线与SN 2015 bn相似，但相对较高。SN 2010 kd具有比PTF 12 dam和SN 2015 bn更高的单区局部热力学平衡温度，其Oi喷出质量上限为1000 M Ω. SN 2010 kd的宿主是一个矮星系，具有高星星形成率（0.18 ± 0.04 M yr−1）和极端的发射线。
This paper presents data and analysis of SN 2010kd, a low-redshift (z = 0.101) H-deficient superluminous supernova (SLSN), based on ultraviolet/optical photometry and optical spectroscopy spanning between −28 and +194 days relative to B-band maximum light. The B-band light-curve comparison of SN 2010kd with a subset of well-studied SLSNe I at comparable redshifts indicates that it is a slow-decaying PTF12dam-like SLSN. Analytical light-curve modeling using the Minim code suggests that the bolometric light curve of SN 2010kd favors circumstellar matter interaction for the powering mechanism. SYNAPPS modeling of the early-phase spectra does not identify broad H or He lines, whereas the photospheric-phase spectra are dominated by O i, O ii, C ii, C iv, and Si ii, in particular the presence of both low- and high-velocity components of O ii and Si ii lines. The nebular-phase spectra of SN 2010kd are dominated by O i and Ca ii emission lines similar to those seen in other SLSNe I. The line velocities in SN 2010kd exhibit flatter evolution curves similar to SN 2015bn but with comparatively higher values. SN 2010kd shows a higher single-zone local thermodynamic equilibrium temperature in comparison to PTF12dam and SN 2015bn, and it has an upper O i ejected mass limit of ∼10 M⊙. The host of SN 2010kd is a dwarf galaxy with a high star formation rate (∼0.18 ± 0.04 M⊙ yr−1) and extreme emission lines.