The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels
复制标题
DOI：
10.3847/1538-4357/ac8ff6
复制
发表时间：
2022-05
期刊：
影响因子：
--
通讯作者：
C. Pellegrino;D. Howell;G. Terreran;I. Arcavi;K. Bostroem;P. Brown;J. Burke;Y. Dong;A. Gil
中科院分区：
文献类型：
--
作者：
C. Pellegrino;D. Howell;G. Terreran;I. Arcavi;K. Bostroem;P. Brown;J. Burke;Y. Dong;A. Gil
我们提出了一个样本的Icn型超新星（SNe Icn），一个新发现的瞬态类的特点是它们的相互作用与H-和He-穷人拱星材料（CSM）。该样本是迄今为止最大的SNe Icn集合，包括对两个已发表物体（SN 2019 hgp和SN 2021 csp）和两个尚未在文献中发表的物体（SN 2019 jc和SN 2021 ckj）的观测。SNe Icn显示了一系列的峰值亮度，上升时间和下降率，以及各种各样的后期光谱特征。为了研究它们的爆炸和祖属性，我们拟合它们的热光变曲线的半分析模型，包括光度输入的拱星相互作用和放射性衰变的56镍。我们从光变曲线推断出低的喷出物质量（102 M）和56 Ni质量（100.04 M），这表明在致密的CSM中正常的剥离包络超新星（SESN）爆炸不可能是SNe Icn的潜在动力机制。此外，我们发现，估计的星星的形成率密度在SN 2019 jc的位置位于低端的SESNe的分布，在冲突的大规模星星的祖先，这个对象。根据其估计的喷出物质量，56 Ni质量和爆炸现场的属性，我们建议一个低质量，超剥离星星作为SN 2019 jc的祖先。对于其他SNe Icn，我们认为沃尔夫-拉叶星星祖先可能会更好地解释它们观察到的特性。这项研究表明，多个祖通道可能会产生SNe Icn和其他相互作用的动力瞬变。
We present a sample of Type Icn supernovae (SNe Icn), a newly discovered class of transients characterized by their interaction with H- and He-poor circumstellar material (CSM). This sample is the largest collection of SNe Icn to date and includes observations of two published objects (SN 2019hgp and SN 2021csp) and two objects not yet published in the literature (SN 2019jc and SN 2021ckj). The SNe Icn display a range of peak luminosities, rise times, and decline rates, as well as diverse late-time spectral features. To investigate their explosion and progenitor properties, we fit their bolometric light curves to a semianalytical model consisting of luminosity inputs from circumstellar interaction and radioactive decay of 56Ni. We infer low ejecta masses (≲2 M ⊙) and 56Ni masses (≲0.04 M ⊙) from the light curves, suggesting that normal stripped-envelope supernova (SESN) explosions within a dense CSM cannot be the underlying mechanism powering SNe Icn. Additionally, we find that an estimate of the star formation rate density at the location of SN 2019jc lies at the lower end of a distribution of SESNe, in conflict with a massive star progenitor of this object. Based on its estimated ejecta mass, 56Ni mass, and explosion site properties, we suggest a low-mass, ultra-stripped star as the progenitor of SN 2019jc. For other SNe Icn, we suggest that a Wolf–Rayet star progenitor may better explain their observed properties. This study demonstrates that multiple progenitor channels may produce SNe Icn and other interaction-powered transients.