Confined Dense Circumstellar Material Surrounding a Regular Type II Supernova: The Unique Flash-Spectroscopy Event of SN 2013fs
O. Yaron, D. A. Perley, A. Gal-Yam, J. H. Groh, A. Horesh, E. O. Ofek, S. R. Kulkarni, J. Sollerman, C. Fransson, A. Rubin, P. Szabo, N. Sapir, F. Taddia, S. B.… 展开作者
O. Yaron, D. A. Perley, A. Gal-Yam, J. H. Groh, A. Horesh, E. O. Ofek, S. R. Kulkarni, J. Sollerman, C. Fransson, A. Rubin, P. Szabo, N. Sapir, F. Taddia, S. B. Cenko, S. Valenti, I. Arcavi, D. A. Howell, M. M. Kasliwal, P. M. Vreeswijk, D. Khazov, O. D. Fox, Y. Cao, O. Gnat, P. L. Kelly, P. E. Nugent, A. V. Filippenko, R. R. Laher, P. R. Wozniak, W. H. Lee, U. D. Rebbapragada, K. Maguire, M. Sullivan, M. T. Soumagnac
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Published in Nature Phys., including methods and SI
With the advent of new wide-field, high-cadence optical transient surveys, our understanding of the diversity of core-collapse supernovae has grown tremendously in the last decade. However, the pre-supernova evolution of massive stars, that sets the physical backdrop to these violent events, is theoretically not well understood and difficult to probe observationally. Here we report the discovery of the supernova iPTF13dqy = SN 2013fs, a mere ~3 hr after explosion. Our rapid follow-up observations, which include multiwavelength photometry and extremely early (beginning at ~6 hr post-explosion) spectra, map the distribution of material in the immediate environment (<~ 10^15 cm) of the exploding star and establish that it was surrounded by circumstellar material (CSM) that was ejected during the final ~1 yr prior to explosion at a high rate, around 10^-3 solar masses per year. The complete disappearance of flash-ionised emission lines within the first several days requires that the dense CSM be confined to within <~ 10^15 cm, consistent with radio non-detections at 70--100 days. The observations indicate that iPTF13dqy was a regular Type II SN; thus, the finding that the probable red supergiant (RSG) progenitor of this common explosion ejected material at a highly elevated rate just prior to its demise suggests that pre-supernova instabilities may be common among exploding massive stars.
Observable Signatures of Supernova Shock Breakout in Confined Circumstellar Medium
National Taiwan University（台湾大学）；Academia Sinica, Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Heidelberger Institut für Theoretische Studien（海德堡理论研究所）；Kyoto University（京都大学）；Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学计算中心）
Radio Emission from Fast Blue Optical Transients Powered by Trans-relativistic Shocks in Confined Circumstellar Material
Central China Normal University（华中师范大学）；Institute of Astrophysics, Central China Normal University（华中师范大学天体物理研究所）；Laboratory for Compact Object Astrophysics and Astronomical Technology, Central China Normal University（华中师范大学致密天体天文学与技术实验室）；Education Research and Application Center, National Astronomical Data Center（国家天文台教育研究与应用中心）
Analytical modeling of polarization signals arising from confined circumstellar material in Type II supernovae
University of Turku（图尔库大学）；Aalto University Metsähovi Radio Observatory（阿尔托大学梅萨霍维射电天文台）；Aalto University Department of Electronics and Nanoengineering（阿尔托大学电子与纳米工程系）；Kyoto University（京都大学）；The University of Tokyo（东京大学）
EP250827b/SN 2025wkm: An X-ray Flash-Supernova Powered by a Central Engine and Circumstellar Interaction
University of Maryland, College Park（马里兰大学帕克分校）；Joint Space-Science Institute, University of Maryland, College Park（马里兰大学联合空间科学研究所）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；California Institute of Technology（加州理工学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Carnegie Mellon University（卡内基梅隆大学）；Massachusetts Institute of Technology（麻省理工学院）；Flatiron Institute（平顿研究所）；Columbia University（哥伦比亚大学）；Cornell University（康奈尔大学）
Radio Constraints on the Circumstellar Environment of the Type IIb Supernova SN 2024iss
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan（水泽VLBI观测站，日本国立天文台）；Astronomical Science Program, Graduate Institute for Advanced Studies, SOKENDAI（先进研究生院天文学项目，SOKENDAI）；Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo（东京大学大学院人文社会系研究科地球行星科学专攻）；Department of Physics, National Chung Hsing University（国立中兴大学物理系）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；The Research Institute for Time Studies, Yamaguchi University（山口大学时计学研究所以）；Graduate School of Science and Technology for Innovation, Yamaguchi University（山口大学创新理工学研究科）；Department of Astronomy, Kyoto University（京都大学宇宙学前沿中心天文学专攻）
Circumstellar Medium of Supernovae as New Probes for Feebly Interacting Particles
Korea Advanced Institute of Science and Technology (KAIST)（韩国科学技术院）；Institute for Basic Science（基础科学研究院）；Academia Sinica（中央研究院）；National Center for Theoretical Sciences（国家理论科学中心）；Kyungpook National University（庆北国立大学）
Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；International Centre of Supernovae, Yunnan Key Laboratory（超新星国际中心，云南省重点实验室）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Department of Astronomy, Kyoto University（京都大学天文学系）；South-Western Institute for Astronomy Research, Yunnan University（云南大学西南天文研究所）；Yunnan Key Laboratory of Survey Science, Yunnan University（云南大学云南省测绘科学重点实验室）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Electronic Science and Engineering, Chongqing University of Posts and Telecommunications（重庆邮电大学电子科学与工程学院）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）
SN 2024acyl 是一种快速、线性衰减的 Type Ibn 超新星，具有早期闪光电离特征，其光谱和光变曲线特征支持由抛射物与 CSM 交互驱动的 SN 模型。
Probing Circumstellar Material and Shock Acceleration in Core-Collapse Supernovae with High-Energy Neutrinos
School of Mathematics and Physics, China University of Geosciences（中国地质大学数学与物理学院）；Shenzhen Research Institute of China University of Geosciences（中国地质大学（深圳）研究院）
SN 2023zcu: A Type IIP SN with Early Flash Features
Aryabhatta Research Institute of Observational Sciences（阿亚巴塔观测科学研究所）；Mahatma Jyotiba Phule Rohilkhand University（马哈特玛·约提巴·普尔罗希尔坎德大学）；European Southern Observatory（欧洲南方天文台）；Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Brera（意大利国家天体物理研究所，布雷拉天文台）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Las Cumbres Observatory（拉斯坎伯斯天文台）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；University of California, Davis（加州大学戴维斯分校）；University of California, Berkeley（加州大学伯克利分校）
SN 2023zcu是一种具有早期闪光特征的IIP型超新星，通过光谱和光度分析确定其前身星质量及距离，揭示了IIP型超新星的物理特性。
SN 2020uem: A Possible Thermonuclear Explosion within A Dense Circumstellar Medium (II) The Properties of The CSM from Polarimetry and Light Curve Modeling
The Eye of Sauron in SN 2025ngs: a Short-plateau Cousin of SN 1998S with Evidence for a Ring-like Circumstellar Medium
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Physics and Astronomy, University of California, Davis（加州大学戴维斯分校物理与天文学系）；Gemini Observatory（Gemini 天文台）；School of Physical and Chemical Sciences – Te Kura Matū, University of Canterbury（坎特伯雷大学物理与化学科学学院）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密松天体物理中心）
SN 2025ngs 是一个介于强相互作用超新星（IIn型）和IIP型之间的短平台超新星，其光谱特征显示与SN 1998S相似，但峰值亮度较低，且有环状周围介质的证据。
SN 2019vxm: A luminous and long-lived Type IIn supernova with early flash-ionisation features
Tsinghua University（清华大学）；Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学（SOKENDAI））；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）
SN 2019vxm是一颗峰值亮度高、演化缓慢的IIn型超新星，早期光谱显示闪光电离特征，后期红外超表明新尘埃形成，其光变曲线与SN 2010jl相似。
The flash-ionised SN Ibn 2025kzr: H-free CSM formed during a precursor outburst 55 days prior to explosion
DTU Space, Technical University of Denmark（丹麦技术大学空间中心）；South African Astronomical Observatory（南非天文台）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；Department of Physics, University of the Free State（自由邦大学物理系）；Department of Physics, Stellenbosch University（斯坦伦布什大学物理系）；Department of Astrophysics/IMAPP, Radboud University（拉德堡德大学天体物理学系/IMAPP）；The Inter-University Institute for Data Intensive Astronomy, University of Cape Town（开普敦大学跨大学数据密集型天文研究所）；Department of Particle Physics and Astrophysics, Weizmann Institute of Science（魏茨曼科学研究所粒子物理与天体物理系）
