发表机构
INAF - Osservatorio Astronomico di Roma; Università Tor Vergata, Dipartimento di Fisica; FSLAC IRL 2009, CNRS/IAC; Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM; Institute of Space Sciences (ICE, CSIC); Institut d’Estudis Espacials de Catalunya (IEEC); Astrophysics Research Institute, Liverpool John Moores University; The Oskar Klein Centre, Department of Astronomy, AlbaNova; Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA); University College London, Mullard Space Science Laboratory; IPAC, California Institute of Technology; Caltech Optical Observatories, California Institute of Technology（罗马天文台意大利国家天体物理研究所; 托尔维尔加塔大学物理系; CNRS/IAC FSLAC IRL 2009; 巴黎萨克雷大学、巴黎西岱大学、CEA、CNRS、AIM; 空间科学研究所（ICE，CSIC）; 加泰罗尼亚太空研究学院（IEEC）; 利物浦约翰摩尔斯大学天体物理研究所; 阿尔巴诺瓦奥斯卡·克莱因中心天文学系; 天体物理学跨学科探索与研究中心（CIERA）; 伦敦大学学院穆拉德空间科学实验室; 加州理工学院IPAC; 加州理工学院帕萨迪纳光学观测站）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过多波段观测分析最邻近的SLSN-Ib SN 2024jlc，发现其低峰值亮度、慢演化及氦富集特征，支持星周介质相互作用和磁星自转模型，并暗示γ射线信号，认为该超新星可能桥接超亮超新星与经典剥离包层超新星。
AI 中文摘要
I型超亮超新星SN~2024jlc（ZTF24aapadbb）于2024年5月25日在红移$z=0.039$处爆发。作为近年来发现的最接近此类超新星的事件，也是历史上最接近的事件之一，它为详细研究这类天体提供了难得的机会。我们进行了多波段分析，覆盖十个数量级的频率范围，包括光学/紫外测光和光谱、软硬X射线以及高能$\gamma$射线。我们将该事件定性为慢演化且富氦的超新星，其峰值光度是超亮事件中报道的最低之一，$M_g\sim-19.37$ mag，光变曲线演化与星周介质相互作用和磁星自转模型均兼容，且$^{56}$Ni衰变有显著贡献。在软硬X射线波段未发现显著超出，我们给出了通量上限。此外，我们分析了两年\textit{Fermi}-LAT数据，报告了一个约$3.6\sigma$水平的$\gamma$射线信号的有趣迹象，但无法确认探测。伽马与光学效率比$\eta=0.38$暗示存在中心引擎场景，类似于SN~2017egm。我们的分析表明，SN~2024jlc可能桥接SLSNe与经典剥离包层超新星。尽管这一桥接尚不完善，但它可能由所有SLSN-Ib超新星构成，关键区别在于供能机制。
英文摘要
The Type I super-luminous supernova SN~2024jlc (ZTF24aapadbb) exploded on the 25th of May 2024 at $z = 0.039$. Being the closest supernova of this class discovered in recent years and one of the closest ever, represented a rare opportunity to study in detail this type of objects. We performed a multi-wavelength analysis, spanning ten orders of magnitude in frequency, including optical/UV photometry and spectroscopy, soft and hard X-rays, and high-energy $γ$-rays. We characterized the event as a slow-evolving and He-rich supernova, with one of the lowest peak luminosities reported for a super-luminous event $M_g\sim-19.37$ mag, and a light curve evolution compatible with both circumstellar interaction and magnetar spin-down models, with noticeable contribution from $^{56}$Ni decay. No significant excess was found in the soft and hard X-ray bands, for which we provide upper-limits on the flux. Additionally, we analyzed two years of \textit{Fermi}-LAT data, from which we report an intriguing hint of a $γ$-ray signal at the $\sim 3.6 σ$ level, although no firm detection can be claimed. The gamma to optical efficiency ratio, $η= 0.38$, is suggestive of the presence of a central-engine scenario, similar to SN~2017egm. Our analysis suggests that SN~2024jlc could bridge the gap between SLSNe and classical stripped-envelope supernovae. While still poorly populated, this bridge could consist of all SLSN-Ib supernovae, with the key difference residing in the powering mechanism.
CommentsPublished on A&A
Journal refA&A, Volume 713, A269, September 2026
DOI：10.1051/0004-6361/202659680
