Two stripped envelope supernovae with circumstellar interaction -- but only one really shows it
J. Sollerman, C. Fransson, C. Barbarino, C. Fremling, A. Horesh, E. Kool, S. Schulze, I. Sfaradi, S. Yang, E. C. Bellm, R. Burruss, V. Cunningham, K. De, A. J. … 展开作者
J. Sollerman, C. Fransson, C. Barbarino, C. Fremling, A. Horesh, E. Kool, S. Schulze, I. Sfaradi, S. Yang, E. C. Bellm, R. Burruss, V. Cunningham, K. De, A. J. Drake, V. Z. Golkhou, D. A. Green, M. Kasliwal, S. Kulkarni, T. Kupfer, R. R. Laher, F. J. Masci, H. Rodriguez, B. Rusholme, D. R. A. Williams, L. Yan, J. Zolkower
We present SN 2019tsf (ZTF19ackjszs) and SN 2019oys (ZTF19abucwzt). These two stripped envelope Type Ib supernovae suddenly showed a (re-)brightening in their late light curves. We investigate this in the context of circumstellar material (CSM) interaction with previously ejected material, a phenomenon that is unusual among SE SNe. We analyse observational data, consisting of optical light curves and spectra. For SN 2019oys we also have detections in radio as well as limits from UV and X-rays. Both light curves show spectacular re-brightening after about 100 days. In the case of SN 2019tsf, the re-brightening is followed by a new period of decline, and the spectra never show signs of narrow emission lines that would indicate CSM interaction. On the contrary, SN 2019oys made a spectral makeover from a Type Ib to a spectrum clearly dominated by CSM interaction at the light curve brightening phase. Deep spectra reveal a plethora of narrow high ionization lines, including coronal lines, and the radio observations show strong emission. The rather similar light curve behaviour indicate CSM interaction as the powering source. For SN 2019oys the evidence for a phase where the ejecta hit H-rich material, likely ejected from the progenitor star, is conspicuous. We observe strong narrow lines of H and He, but also a plethora of high ionization lines, including coronal lines, revealing shock interaction. Spectral simulations of SN 2019oys show two distinct density components, one with density > 1e9/cm3, dominated by somewhat broader, low ionization lines of H I, He I, Na I and Ca II, and one with narrow, high ionization lines at a density about 1e6 /cm3. The former is strongly affected by electron scattering. The evidence for CSM interaction in SN 2019oys is corroborated by detections in radio. On the contrary, for SN 2019tsf, we find little evidence in the spectra for any CSM interaction.
An optimized radio follow-up strategy for stripped-envelope core-collapse supernovae
几个正在进行或计划进行的天气光学调查提供或即将提供一个前所未有的机会，发现更大的样本的最罕见类型的剥离信封核心坍缩超新星（SNe），如那些与相对论喷流，轻度相对论喷出物，或强相互作用与星周介质（CSM）。无线电波长的观测是探测最快移动的喷出物以及更密集的星周环境的有用工具，因此可以帮助我们识别最罕见的核心塌陷爆炸类型。在这里，我们将讨论如何建立一个有效的无线电后续程序，以检测和正确识别无线电发射剥离信封核心崩溃爆炸。我们使用一种类似于\citealt{Carbone2018}中描述的方法，并确定GHz射电观测的最佳定时，假设灵敏度与Karl G. Jansky甚大阵。进行优化是为了确保收集到的射电观测可以通过使用尽可能少的望远镜时间来识别为射电对应物提供动力的爆炸类型。我们还提出了一个以前未发表的上限的晚期射电辐射超新星iPTF17cw。最后，我们通过讨论X射线的后续影响得出结论。
Diversity of stripped-envelope supernova light curves from interaction with binary-driven circumstellar material
Institute of Science and Technology Austria（奥地利科学技术研究院）；Heidelberger Institut für Theoretische Studien（海德堡理论研究所）；Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut（海德堡大学天文学中心计算天文研究所）；Department of Physics, University of Oxford（牛津大学物理系）；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（SOKENDAI高级研究生院）；School of Physics and Astronomy, Monash University（莫纳什大学物理与天文学院）；Institute of Astronomy, KU Leuven（荷语鲁汶大学天体物理学研究所）；Leuven Gravity Institute, KU Leuven（荷语鲁汶大学勒芬引力研究所）；Anton Pannekoek Institute of Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天体物理学研究所）
Hydrogen-Rich to Stripped-Envelope:Observational Continuity and Biases in CCSNe
Department of Astronomy, Oskar Klein Center, Stockholm University（斯德哥尔摩大学奥斯卡·克莱因中心天文学系）；Astrophysics Division, National Centre for Nuclear Research（国家核研究中心天体物理部）
Late-Time HST UV Detections Reveal Eruptive Mass Loss and Circumstellar Interaction in a Quarter of Stripped-Envelope Supernovae
California Institute of Technology（加州理工学院）；Stockholm University（斯德哥尔摩大学）；Columbia University（哥伦比亚大学）；National Central University（中央大学）；Weizmann Institute of Science（魏茨曼科学研究所）
A unified accreting magnetar model for long-duration gamma-ray bursts and some stripped-envelope supernovae
长期的伽马射线暴（LGRB）和I型超亮超新星（SLSNe~I）都被认为是由中心磁星提供能量的。的相关性，提出了初始自旋周期（$P_0$）和表面磁场（$B$）的磁星供电的X射线平台在LGRB余辉之间，表明磁星已经达到了平衡自旋周期由于回落吸积的可能性。相应的吸积速率被推断为$\dot{M}\approx10^{-4}-10^{-1}$ M $_\odot$ s $^{-1}$，这一结果对各向同性磁星风和平行磁星风都成立。对于SLSNe~I和一部分发动机驱动的正常Ic型超新星（SNe~Ic）和宽线亚类（SNe~Ic-BL），磁星也可以达到吸积诱导的自旋平衡，但相应的$B-P_0$分布表明吸积速率范围不同，即，$\dot{M}\approx 10^{-7}-10^{-3}$ M $_\odot$ s $^{-1}$。考虑回退吸积效应，磁场相对较弱的磁星导致SLSNe~I，而磁场较强的磁星导致SNe~Ic/Ic-BL。在我们的样本中，一些SLSNe~I可能来自紧凑的祖星，而另一些需要较长时间吸积的可能来自具有更多扩展包层或星周介质的祖星。
Decadal pre-explosion activity and circumstellar interaction in a supernova
National Central University（国立中央大学）；Henan Academy of Sciences（河南省科学院）；University of Oxford（牛津大学）；National Astronomical Observatory of Japan（日本国立天文台）；SOKENDAI（综合研究大学院大学）；Monash University（蒙纳士大学）；Aarhus University（奥胡斯大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；The Australian National University（澳大利亚国立大学）
Late-time H/He-poor circumstellar interaction in the type-Ic supernova SN 2021ocs: an exposed oxygen-magnesium layer and extreme stripping of the progenitor
Late-time evolution of the interacting stripped-envelope supernova 2017dio
University of Turku（图尔库大学）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚太空研究学院（IEEC））；Finnish Centre for Astronomy with ESO (FINCA)（芬兰ESO天文中心（FINCA））；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）；Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa（里斯本大学理学院，天体物理与空间科学研究所）；Department of Astronomy, Kyoto University（京都大学天文学系）
Supernovae interacting with Si and S-rich circumstellar matter from double white dwarf mergers
National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，日本国立科学研究所）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学）；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学学院）；International Center of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research, Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台超新星国际研究中心（ICESUN），云南省超新星研究重点实验室）
Shock cooling emission from late-time mass loss in low-mass He star binaries
The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Physics & Astronomy, Northwestern University（西北大学天体物理交叉探索与研究中心）
SN~2018erx: A fast-evolving, dust-reddened Type Icn supernova with broad C II emission lines
California Institute of Technology（加州理工学院）；Stockholm University（斯德哥尔摩大学）；Liverpool John Moores University（利物浦约翰摩尔斯大学）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理学跨学科探索与研究中心）；University of Minnesota（明尼苏达大学）；Columbia University（哥伦比亚大学）；Flatiron Institute（平托研究所）；Weizmann Institute of Science（魏茨曼科学研究所）
Nebular Spectra of the Extremely Metal-Poor SN II 2023ufx Over a Year After Explosion: A Massive Progenitor and Unique Circumstellar Environment
Center for Cosmology and AstroParticle Physics（宇宙学与暗物质粒子物理中心）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Institut d’Astrophysique de Paris, CNRS-Sorbonne Université（巴黎天体物理学研究所，法国国家科学研究中心-索邦大学）；French-Chilean Laboratory for Astronomy, IRL 3386, CNRS, Instituto de Astrofísica, Pontificia Universidad Católica de Chile（法智利天文学联合实验室，法国国家科学研究中心，智利天主教Pontificia大学天体物理研究所）
The hydrogen-free circumstellar interaction in the Type Ib supernova 2021efd: A clue to the mechanism of the helium-layer stripping
University of Turku（图尔库大学）；Nordic Optical Telescope（北欧光学望远镜）；Aalto University（阿尔托大学）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究所）；Finnish Center of Astronomy with ESO (FINCA)（芬兰ESO天文学中心）；Aarhus University（奥胡斯大学）；Kyoto University（京都大学）；Zhejiang University（浙江大学）
