多波段识别一颗由双星驱动的超新星前质量损失与星周物质相互作用供能的光亮中红外超新星
Multi-Wavelength Identification of a Luminous Mid-Infrared Supernova Powered by Circumstellar Interaction with Binary-Driven Pre-supernova Mass Loss
- Columbia University（哥伦比亚大学）
- Center for Computational Astrophysics, Flatiron Institute（西蒙斯基础研究所计算天体物理中心）
- California Institute of Technology（加州理工学院）
- The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过多波段观测SN 2022yyz，利用红外测光选择发现晚期星周物质相互作用，结合模型揭示双星驱动的超新星前质量损失增强，为绘制大质量恒星终局质量损失奠定基础。
AI中文摘要：
大质量恒星的终局质量损失通常通过核心坍缩超新星（CCSNe）中的星周物质相互作用观测来重建；然而，这类特征可能因其出现的相位不同而容易被遗漏。本文对SN 2022yyz进行了多波段研究，这是一颗邻近的CCSNe，通过其在NEOWISE中发现的发光晚期中红外（MIR）超额（在发现后>500天）而被选中。该超新星在发现时被分类为II型，其峰值热光度达到1.3^{+0.7}_{-0.4}×10^{43} erg s^{-1}，随后光变曲线在约300天时下降并逐渐消失。我们展示了在约1200天时的晚期HST/WFC3紫外（UV）成像和Keck/LRIS光谱，这些观测通过紫外超额（与强MgII贡献一致）和扁平顶Hα谱线轮廓清晰揭示了星周介质（CSM）相互作用的迹象。我们表明，热光变曲线和晚期紫外光度可以用一个涉及破碎幂律密度轮廓的半解析CSM相互作用模型来解释：在约10^{16} cm半径内存在约2.7 M_sun的邻近致密CSM，其外围被质量损失率约10^{-4} M_sun yr^{-1}的类风状CSM包围。破碎密度轮廓表明，在爆炸前几百年开始质量损失率增强了约100倍以上，指向双星系统中可能的公共包层抛射事件。尽管在如此近的距离上被忽视而未被后续观测，我们的结果表明，红外测光选择方法为绘制大质量恒星的终局质量损失提供了强大途径——为罗马空间望远镜巡天奠定了基础。
英文摘要：
Terminal mass-loss in massive stars is commonly reconstructed from observations of circumstellar interaction in core-collapse supernovae (CCSNe); however, such signatures can be easily missed depending on the phase when they appear. In this paper, we present a multi-wavelength study of SN\,2022yyz, a nearby CCSN selected by its luminous late-time mid-infrared (MIR) excess in NEOWISE at $> 500$ days after the discovery. Classified as a Type II SN at discovery, it reached a peak bolometric luminosity of $1.3^{+0.7}_{-0.4}\times10^{43}$ erg s$^{-1}$ before fading away with a light-curve drop at $\sim 300$ days. We present late-time HST/WFC3 ultraviolet (UV) imaging and Keck/LRIS spectroscopy at $\sim 1200$ days, which reveal clear signs of circumstellar-medium (CSM) interaction via a UV excess consistent with a strong MgII contribution and a flat-topped H$α$ profile. We show that the bolometric light curve and the late-time UV luminosity can be explained using a semi-analytic CSM interaction model involving a broken power-law density profile: with $\sim 2.7~M_\odot$ of nearby, dense CSM within a radius of $\sim 10^{16}$ cm surrounded by wind-like outer CSM with a mass-loss rate of $\sim 10^{-4} {\rm ~M_\odot~yr}^{-1}$. The broken density profile indicates $\gtrsim 100\times$ mass-loss rate enhancement starting a few hundred years before explosion, pointing to a possible common-envelope ejection in a binary system. Despite being overlooked for follow-up at such proximity, our results demonstrate that IR photometric selection methods provide a powerful way of mapping terminal mass-loss in massive stars - laying the groundwork for the Roman Space Telescope surveys.
