发表机构
University of North Carolina Chapel Hill; Space Telescope Science Institute; Steward Observatory, University of Arizona; University of Virginia; Pontificia Universidad Católica de Chile; CNRS-Sorbonne Université; California Institute of Technology（北卡罗来纳大学教堂山分校; 太空望远镜科学研究所; 亚利桑那大学斯蒂沃德天文台; 弗吉尼亚大学; 智利天主教 Pontificia 大学; 法国国家科学研究中心-索邦大学; 加州理工学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用JWST在SN 1983V爆发40多年后探测到其尘埃储库，表明双星相互作用形成的环面尘埃被激波加热，贡献宇宙尘埃。光谱观测可最终确认。
AI 中文摘要
搜寻超新星（SNe）的晚期辐射是一个活跃的研究领域。红外（IR）波段对尘埃的热辐射敏感，可用于探测超新星对宇宙尘埃总量的贡献以及前身星的质量损失历史。超新星越古老，其现存尘埃越可能已冷却至大多数天文台（甚至JWST）的探测阈值以下。因此，对超新星进行历时数十年的红外观测极为罕见。在此，我们报告了幸运且偶然的JWST红外观测结果，该观测在Ic型超新星SN 1983V爆发40多年后，在其位置探测到一个点源。我们证明该源与附近的HII区不同，很可能是尘埃超新星。我们还进一步展示了来自哈勃空间望远镜（HST）档案数据的证据，表明存在一个与正在进行的超新星激波相互作用相关的H/alpha对应体，该相互作用通过碰撞加热尘埃。在此情景下，尘埃分布在环面中，这比球状星风更符合双星相互作用引起的质量损失。虽然SN 1983V并非JWST探测到的最古老超新星（SN 1980K），但它紧随其后。此外，它具有相对较大的尘埃质量（约7.7 x 10^-3 M_太阳），特别是对于剥离包层超新星而言。尽管这些尘埃不太可能是新形成的，但它确实表明此类系统可能对尘埃产生有所贡献，尤其是在早期宇宙中，那时大质量恒星和双星系统更为普遍。光谱观测最终可以确认该源的超新星性质。
英文摘要
Searching for late-time emission from supernovae (SNe) is an active field. Infrared (IR) wavelengths are sensitive to thermal emission from dust, which can be used to probe SN contributions to the cosmic dust budget and progenitor mass-loss histories. The older an SN, the more likely it is for any existing dust to have cooled below the detection threshold of most observatories, even JWST. Decades-old IR observations of SNe are therefore exceedingly rare. Here we present fortuitous and serendipitous JWST IR observations that detect a point source at the position of the Type Ic SN 1983V more than 40 yr post-explosion. We demonstrate that the source is unlike nearby HII regions and likely to be the dusty SN. We further show evidence from archival HST data of a plausible H/alpha counterpart associated with ongoing SN shock interaction that collisionally heats the dust. In this scenario, the dust is distributed in a torus, more consistent with mass loss from binary interaction than a spherical wind. While not the oldest SN detected by JWST (SN 1980K), SN 1983V is a close second. Moreover, it has a relatively large dust mass (~7.7 x 10^-3 M_solar), particularly for a stripped-envelope SN. Although the dust is not likely newly formed, it does suggest such systems may contribute to dust production, particularly in the early Universe where massive stars and binary systems were more common. Spectroscopic observations can ultimately confirm the SN nature of this source.
Comments20 pages, 12 figures, 4 tables
