AT 2018dyk: tidal disruption event or active galactic nucleus? Follow-up observations of an extreme coronal line emitter with the Dark Energy Spectroscopic Instrument
Peter Clark, Joseph Callow, Or Graur, Claire Greenwell, Lei Hu, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Kyle Dawson, Axel d… 展开作者
Peter Clark, Joseph Callow, Or Graur, Claire Greenwell, Lei Hu, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Kyle Dawson, Axel de la Macorra, Peter Doel, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Ignasi Pérez-Ràfols, Eusebio Sanchez, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin A. Weaver, Hu Zou
备注：
44 pages, 17 total figures. Author compiled version of the paper now published in MNRAS
通过暗能量光谱仪后续观测和宿主星系分析，确认 AT 2018dyk 是发生在富气体环境中的潮汐瓦解事件，并发现此类 TDE 的中红外特性与局部环境物质含量及密度相关。
摘要：
我们对潮汐瓦解事件（TDE）候选体 AT 2018dyk 的本质提出了新见解。AT 2018dyk 在文献中引发了关于其分类的争论，即它究竟是真正的 TDE 还是活动星系核（AGN）转向状态变化。使用暗能量光谱仪（Dark Energy Spectroscopic Instrument）获取的新后续光谱，结合使用档案 SDSS-MaNGA 数据进行的宿主星系分析，支持将 AT 2018dyk 鉴定为 TDE。具体而言，我们将该天体分类为发生在富气体环境中的 TDE，该环境导致了其中红外（MIR）爆发和 Fe 冕发射线的发展。通过与已知的 TDE 相关极冕线发射体（TDE-ECLEs）样本以及其他显示冕发射线的 TDE（CrL-TDEs）进行比较，揭示了相似的特征和共同属性。例如，两组的中红外特性似乎形成了一个连续体，并与它们局部环境中物质含量和密度有关。这包括在发生在这种富气体环境中的 TDE 存在中红外颜色-光度关系的证据，其中具有更大中红外爆发的也表现出更红的峰值。
英文摘要：
We present fresh insights into the nature of the tidal disruption event (TDE) candidate AT 2018dyk. AT 2018dyk has sparked a debate in the literature around its classification as either a bona-fide TDE or as an active galactic nucleus (AGN) turn-on state change. A new follow-up spectrum taken with the Dark Energy Spectroscopic Instrument, in combination with host-galaxy analysis using archival SDSS-MaNGA data, supports the identification of AT 2018dyk as a TDE. Specifically, we classify this object as a TDE that occurred within a gas-rich environment, which was responsible for both its mid-infrared (MIR) outburst and development of Fe coronal emission lines. Comparison with the known sample of TDE-linked extreme coronal line emitters (TDE-ECLEs) and other TDEs displaying coronal emission lines (CrL-TDEs) reveals similar characteristics and shared properties. For example, the MIR properties of both groups appear to form a continuum with links to the content and density of the material in their local environments. This includes evidence for a MIR colour-luminosity relationship in TDEs occurring within such gas-rich environments, with those with larger MIR outbursts also exhibiting redder peaks.
Temporal Variation of the Coronal Radius Parameter in a Jetted Tidal Disruption Event: Swift J1644+57
University of Manitoba（曼尼托巴大学）；Chungbuk National University（忠北国立大学）；Aoyama Gakuin University（青山学院大学）；Physical Research Laboratory（物理研究实验室）；Indian Centre for Space Physics（印度空间物理中心）；Indian Institute of Astrophysics（印度天体物理研究所）；INAF-IASF Palermo（意大利国家天体物理研究所巴勒莫天体物理研究所）；University of British Columbia（不列颠哥伦比亚大学）；SRM University-AP（SRM大学安得拉邦校区）
VLASS tidal disruption events with optical flares II: discovery of two TDEs with intermediate width Balmer emission lines and connections to the ambiguous extreme coronal line emitters
Discovery of Quasi-periodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: implications for the QPE/TDE fraction and a connection to ECLEs
NTT, Spitzer and Chandra spectroscopy of SDSSJ095209.56+214313.3: the most luminous coronal-line supernova ever observed, or a stellar tidal disruption event ?
Early results in the search for extreme coronal line emitters with the Dark Energy Spectroscopic Instrument
University of Southampton（南安普顿大学）；Institute of Cosmology and Gravitation, University of Portsmouth（朴茨茅斯宇宙学与引力研究所）；American Museum of Natural History（美国自然历史博物馆）；University of California, Berkeley（加州大学伯克利分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）；University of Rochester（罗切斯特大学）
ATLAS22kjn (AT 2022fpx): A Coronal Line Emitter with an Early Light Curve Bump and Mid-Infrared Dust Echo
University of Illinois（伊利诺伊大学）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天文研究所）；School of Physics, University of Melbourne（墨尔本大学物理学院）；The Ohio State University（俄亥俄州立大学）；Texas Tech University（德克萨斯理工大学）；Peking University（北京大学）；National Astronomical Observatories, Chinese Academy of Science（中国科学院国家天文台）
Rapid onset of a Comptonisation zone in the repeating tidal disruption event XMMSL2 J140446.9-251135
Telespazio UK for ESA（ESA英国泰莱斯帕齐奥）；Schmidt Sciences（施密特科学）；Space Telescope Science Institute（太空望远镜科学研究所）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；University of Arizona（亚利桑那大学）；Max-Planck-Institut für extraterrestrische Physik（马普地外物理研究所）；University of Hertfordshire（赫特福德大学）；University of Oxford（牛津大学）；Centro de Astrobiología (CAB), CSIC-INTA（CSIC-INTA天体生物学中心）；ESA（欧洲空间局）；SERCO for ESA（ESA塞科服务）
eROSITA-RU Tidal Disruption Events with Keck-I/LRIS: Sample Selection, Optical Properties, and Host Galaxy Demographics
University of California, Berkeley（加州大学伯克利分校）；Sichuan University（四川大学）；Miller Institute for Basic Research in Science（米勒基础科学研究学院）；Berkeley Center for Multi-messenger Research on Astrophysical Transients and Outreach (Multi-RAPTOR)（伯克利多信使天体物理瞬变现象研究与外展中心（Multi-RAPTOR））；Space Research Institute (IKI), Russian Academy of Sciences（俄罗斯科学院空间研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
The Radio Properties of Extreme Coronal Line Emitters: Constraints on the Sub-parsec Environment
University of Arizona（亚利桑那大学）；University of Utah（犹他大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；University of California, Berkeley（加利福尼亚大学伯克利分校）；Stanford University（斯坦福大学）
Back from the dead: AT2019aalc as a candidate repeating TDE in an AGN
Ruhr Astroparticle and Plasma Physics Center (RAPP Center)（鲁尔天体物理与等离子体物理中心）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Deutsches Elektronen-Synchrotron (DESY)（德国电子同步辐射中心）；Institut fur Physik, Humboldt-Universität zu Berlin（柏林洪堡大学物理研究所）；Division of Physics, Mathematics, and Astronomy, California Institute of Technology（加州理工学院物理、数学和天文学系）；University of Maryland, Department of Astronomy（马里兰大学天文学系）；NASA Goddard Space Flight Center, Astrophysics Science Division（美国宇航局戈达德太空飞行中心天体物理学科学部）；Center for Research and Exploration in Space Science and Technology, NASA/GSFC（NASA/GSFC空间科学与技术研究探索中心）
