SN 2019cqc：呈现电子散射特征的富氢超亮超新星
SN 2019cqc: A Hydrogen-rich Superluminous Supernova Showing Electron-Scattering Signatures
- Manipal Academy of Higher Education（马尼帕尔高等教育学院）
- Institute of Astronomy Space and Earth Science (IASES)（天体空间与地球科学研究所）
- Queen’s University Belfast（贝尔法斯特女王大学）
- European Southern Observatory（欧洲南方天文台）
- University of Warsaw（华沙大学）
- Las Cumbres Observatory（拉斯坎伯斯天文台）
- University of California, Santa Barbara（加州大学圣塔芭芭拉分校）
- University of Turku（图尔库大学）
- European University Cyprus（塞浦路斯欧洲大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究对富氢超亮超新星SN 2019cqc开展测光与光谱观测，借助MOSFiT建模发现其能量源于星周介质相互作用，揭示其前身星为亮蓝变星，还观测到Hα线的不对称性及4600Å处的短期特征。
AI中文摘要：
无窄发射线的富氢超亮超新星（SLSNe-II）是一类罕见的暂现天体，其能量机制仍存在争议，尤其是星周介质（CSM）相互作用的作用。我们报告SN 2019cqc的测光和光谱观测结果，以探究其能量来源与前身星质量损失情况。我们使用MOSFiT工具，结合csm和csmni模型对光变曲线进行建模，以约束爆炸和星周介质参数。SN 2019cqc的峰值绝对星等$M_g=-20.21\rm{\textpm}0.07$，以辐射形式释放的能量约为$1.7\times10^{50}\rm{erg}$。测光与光谱建模表明，两种模型下均以星周介质相互作用为主导，最佳拟合的星周介质质量约为$4.5M_\text{\textodot}$，抛射物质量约为$32M_\text{\textodot}$。推断的星周介质特性显示，在核心坍缩前的数年间，前身星经历了约$0.2-0.3M_\text{\textodot}\rm{yr^{-1}}$的极端爆发式质量损失，这与亮蓝变星类型的变异性状前身星一致。我们观测到H$\text{\textalpha}$发射线存在持续的蓝移不对称性：在早期（$\text{\textlesssim}+110\rm{d}$），该特征归因于电子与抛射物整体速度的散射；在晚期（$\text{\textgtrsim}+402\rm{d}$及之后），其轮廓表明抛射物中随后形成了尘埃。此外，我们在约4600Å处识别出一个独特的短期特征，可能是SN激波与延伸大气相互作用产生的电离C III/N III线的混合。
英文摘要：
Hydrogen-rich superluminous supernovae without narrow emission lines (SLSNe-II) are rare transients whose powering mechanisms remain debated, particularly the role of circumstellar medium (CSM) interaction. We present photometric and spectroscopic observations of SN 2019cqc to investigate its power source and progenitor mass loss. We model the lightcurve using MOSFiT with the csm and csmni models to constrain the explosion and CSM parameters. SN 2019cqc peaked at $M_g = -20.21 \pm 0.07$ and emitted $\sim 1.7 \times 10^{50}\,\mathrm{erg}$ of energy in the form of radiation. Photometric and spectroscopic modeling indicates that CSM interaction dominates in both scenarios, with best-fit CSM and ejecta masses of $\sim 4.5~ M_\odot$ and $\sim 32~ M_\odot$, respectively. The inferred CSM properties imply an extreme eruptive mass loss at a rate of $\sim 0.2--0.3 ~M_\odot\,\mathrm{yr^{-1}}$ in the years preceding the core collapse, consistent with a variable progenitor of luminous blue variable progenitor. We observe a persistent blueshifted asymmetry in the H$α$ emission line. At early times ($\lesssim +110$~d), this is attributed to electron scattering with bulk Velocity of ejecta, while the profile at late epochs ($\gtrsim +402$~d onward) suggests the subsequent formation of dust in the ejecta. Additionally, we identify a distinct, short-lived feature at $\sim$ 4600 Å , likely a blend of ionized C III/N III lines powered by the interaction of the SN-shock with the extended atmosphere.
