本文研究了良映射双峰发射体（AGN with broad double-peaked low-ionization emission lines）3C390.3的宽发射线区结构。除了理论盘模型对3C390.3的双峰宽光学巴耳末线的最佳拟合结果外，我们还试图找到另一种方法来进一步证实双峰线起源于吸积盘。利用AGN WATCH计划1995年前后光学波段的长周期观测光谱，较好地确定了椭圆吸积盘模型（Eracleous et al. 1995）假设的盘状BLR的理论盘参数。通过理论上的盘状BLR，基于混响映射技术可以很好地再现3C390.3宽双峰H $α$的实测光变曲线特征。因此，吸积盘模型是一个更好的模型为3C390.3的BLR的首选。此外，我们还发现，不同的盘参数会导致3C 390. 3的BLR大小与观测数据测量的结果不同，这表明所测量的盘参数对3C 390. 3是有效的。在此基础上，考虑了理论椭圆盘状BLR的进动，我们发现理论模型在2000年的预期谱线轮廓与HST在2000年前后观测到的谱线轮廓是一致的。根据这些结果，我们进一步认为3C390.3的宽双峰Balmer发射线来源于中心黑洞周围的吸积盘。
英文摘要：
In this manuscript, the structure of broad emission line regions (BLRs) of well-mapping double-peaked emitter (AGN with broad double-peaked low-ionization emission lines) 3C390.3 is studied. Besides the best fitted results for double-peaked broad optical balmer lines of 3C390.3 by theoretical disk model, we try to find another way to further confirm the origination of double-peaked line from accretion disk. Based on the long-period observed spectra in optical band around 1995 collected from AGN WATCH project, the theoretical disk parameters of disk-like BLRs supposed by elliptical accretion disk model (Eracleous et al. 1995) have been well determined. Through the theoretical disk-like BLRs, characters of observed light-curves of broad double-peaked H$α$ of 3C390.3 can be well reproduced based on the reverberation mapping technique. Thus the accretion disk model is preferred as one better model for BLRs of 3C390.3. Furthermore, we can find that different disk parameters should lead to some different results about size of BLRs of 3C390.3 from the one measured through observational data, which indicates the measured disk parameters are significantly valid for 3C390.3. After that, the precession of theoretical elliptical disk-like BLRs being considered, we can find that the expected line profile in 2000 by theoretical model is consistent with the observed line profile by HST around 2000. Based on the results, we can further believe that the origination of broad double-peaked balmer emission lines of 3C390.3 are from accretion disk around central black hole.
ABCD: The Nuclear Structure of the Little Red Dots Revealted through Absorption, Break, Continuum, and Decrement
Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究院）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Max-Planck-Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理研究所）
The transient event in NGC 1566 from 2017 to 2019 -- I. An eccentric accretion disk and a turbulent, disk-dominated broad-line region unveiled by double-peaked Ca II and O I lines
本文通过分析 NGC 1566 的光谱变源数据，首次探测到 AGN 中 OI 和 CaII 的宽双峰发射线，揭示其宽线区由相对论偏心吸积盘主导并存在标高湍流分层，蓝移漂移或源于暂现事件期间发射的低光学深度风。
SN 2024iss: A Double-peaked Type IIb Supernova with Evidence of Circumstellar Interaction
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学与空间科学学院）；Las Cumbres Observatory（拉斯坎布拉观测站）；University of California, Santa Barbara（加州大学圣塔芭芭拉分校）；Università degli Studi di Padova（帕多瓦大学）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布里埃拉天文台）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文学系）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；International Centre of Supernovae, Yunnan Key Laboratory（国际超新星研究中心（云南省重点实验室））；Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；Department of Physics, Tsinghua University（清华大学物理系）
A Changing-Look Seyfert Discovered by eROSITA Reveals a Two-Component Broad-Line Region
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院 Nicolaus Copernicus 天文学中心）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所 (AIP)）；Institute of Astronomy, University of Cambridge（剑桥大学天体物理研究所）；Center for Theoretical Physics, Polish Academy of Sciences（波兰科学院理论物理中心）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Department of Physics, University of Johannesburg（约翰内斯堡大学物理系）；Dr. Karl Remeis-Observatory and Erlangen Centre for Astroparticle Physics, Friedrich-Alexander Universität Erlangen-Nürnberg（弗里德里希·阿列克桑德埃尔朗根-纽伦堡大学 Dr. Karl Remeis 天文台和埃尔朗根天体粒子物理中心）；Inter-University Centre for Astronomy and Astrophysics（跨大学天文学与天体物理学中心）；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）；Universität Potsdam（波茨坦大学）；Department of Physics and Astronomy, University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校物理与天文学系）；Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理研究所）
