A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018
Changing-look active galactic nuclei (CL-AGNs), characterized by the emergence or disappearance of broad lines accompanied by extreme continuum flux variability, have drawn much attention for their potential to reveal physical processes underlying AGN evolution. We perform seven-season spectroscopic...
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IOP Publishing
2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4365/ad9a5a |
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| author | Kai-Xing Lu Yan-Rong Li Qingwen Wu Luis C. Ho Zhi-Xiang Zhang Hai-Cheng Feng Sha-Sha Li Yong-Jie Chen Mouyuan Sun Xinwen Shu Wei-Jian Guo Cheng Cheng Jian-Guo Wang Dongchan Kim Jian-Min Wang Jin-Ming Bai |
| author_facet | Kai-Xing Lu Yan-Rong Li Qingwen Wu Luis C. Ho Zhi-Xiang Zhang Hai-Cheng Feng Sha-Sha Li Yong-Jie Chen Mouyuan Sun Xinwen Shu Wei-Jian Guo Cheng Cheng Jian-Guo Wang Dongchan Kim Jian-Min Wang Jin-Ming Bai |
| author_sort | Kai-Xing Lu |
| collection | DOAJ |
| description | Changing-look active galactic nuclei (CL-AGNs), characterized by the emergence or disappearance of broad lines accompanied by extreme continuum flux variability, have drawn much attention for their potential to reveal physical processes underlying AGN evolution. We perform seven-season spectroscopic monitoring on Mrk1018, one of the earliest identified CL-AGN. Around 2020, we detect a full-cycle changing-look transition of Mrk 1018 within one year, associated with a nucleus outburst, which likely arose from the disk instability in the transition region between the outer standard rotation-dominated disk and inner advection-dominated accretion flow. Over the past 45 years, the accretion rate of Mrk 1018 changed 1000 times and the maximum Eddington ratio reached 0.02. By investigating the relation between the broad-line properties and the Eddington ratio ( L _bol / L _Edd ), we find strong evidence that the full-cycle-type transition is regulated by accretion. There exists a turnover point in the Balmer decrement, which is observed for the first time. The broad Balmer lines change from a single peak in Types 1.0–1.2 to double peaks in Types 1.5–1.8, and the double-peak separation decreases with increasing accretion rate. We also find that the FWHM of the broad Balmer lines obeys FWHM $\propto \,{({L}_{{\rm{bol}}}/{L}_{{\rm{Edd}}})}^{-0.27}$ , as expected for a virialized broad-line region (BLR). The velocity dispersion σ _line follows a similar trend in Types 1.5–1.8 but displays a sharp increase in Types 1.0–1.2, resulting in a dramatic drop in FWHM/ σ _line . These findings suggest that a virialized BLR together with accretion-dependent turbulent motions might be responsible for the diversity of BLR phenomena across the AGN population. |
| format | Article |
| id | doaj-art-1052eff84baa4bbfbcd3dd49a50708a7 |
| institution | OA Journals |
| issn | 0067-0049 |
| language | English |
| publishDate | 2025-01-01 |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-1052eff84baa4bbfbcd3dd49a50708a72025-08-20T02:08:15ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127625110.3847/1538-4365/ad9a5aA Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018Kai-Xing Lu0https://orcid.org/0000-0002-2310-0982Yan-Rong Li1https://orcid.org/0000-0001-5841-9179Qingwen Wu2https://orcid.org/0000-0003-4773-4987Luis C. Ho3https://orcid.org/0000-0001-6947-5846Zhi-Xiang Zhang4https://orcid.org/0000-0002-2419-6875Hai-Cheng Feng5https://orcid.org/0000-0002-1530-2680Sha-Sha Li6https://orcid.org/0000-0003-3823-3419Yong-Jie Chen7https://orcid.org/0000-0003-4280-7673Mouyuan Sun8https://orcid.org/0000-0002-0771-2153Xinwen Shu9https://orcid.org/0000-0002-7020-4290Wei-Jian Guo10https://orcid.org/0000-0001-9457-0589Cheng Cheng11https://orcid.org/0000-0003-0202-0534Jian-Guo Wang12https://orcid.org/0000-0003-4156-3793Dongchan Kim13https://orcid.org/0000-0001-7294-106XJian-Min Wang14https://orcid.org/0000-0001-9449-9268Jin-Ming Bai15Yunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People’s Republic of China ; lukx@ynao.ac.cn; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650011, People’s Republic of ChinaKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People’s Republic of ChinaDepartment of Astronomy, School of Physics, Huazhong University of Science and Technology , Luoyu Road 1037, Wuhan, People’s Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of China; Department of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of ChinaDepartment of Astronomy, Xiamen University , Xiamen, Fujian 361005, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People’s Republic of China ; lukx@ynao.ac.cn; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650011, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People’s Republic of China ; lukx@ynao.ac.cn; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650011, People’s Republic of ChinaKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People’s Republic of ChinaDepartment of Astronomy, Xiamen University , Xiamen, Fujian 361005, People’s Republic of ChinaDepartment of Physics, Anhui Normal University , Wuhu, Anhui 241002, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of ChinaChinese Academy of Sciences South America Center for Astronomy , National Astronomical Observatories, CAS, Beijing 100101, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People’s Republic of China ; lukx@ynao.ac.cn; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650011, People’s Republic of ChinaNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USAKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People’s Republic of China ; lukx@ynao.ac.cn; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650011, People’s Republic of ChinaChanging-look active galactic nuclei (CL-AGNs), characterized by the emergence or disappearance of broad lines accompanied by extreme continuum flux variability, have drawn much attention for their potential to reveal physical processes underlying AGN evolution. We perform seven-season spectroscopic monitoring on Mrk1018, one of the earliest identified CL-AGN. Around 2020, we detect a full-cycle changing-look transition of Mrk 1018 within one year, associated with a nucleus outburst, which likely arose from the disk instability in the transition region between the outer standard rotation-dominated disk and inner advection-dominated accretion flow. Over the past 45 years, the accretion rate of Mrk 1018 changed 1000 times and the maximum Eddington ratio reached 0.02. By investigating the relation between the broad-line properties and the Eddington ratio ( L _bol / L _Edd ), we find strong evidence that the full-cycle-type transition is regulated by accretion. There exists a turnover point in the Balmer decrement, which is observed for the first time. The broad Balmer lines change from a single peak in Types 1.0–1.2 to double peaks in Types 1.5–1.8, and the double-peak separation decreases with increasing accretion rate. We also find that the FWHM of the broad Balmer lines obeys FWHM $\propto \,{({L}_{{\rm{bol}}}/{L}_{{\rm{Edd}}})}^{-0.27}$ , as expected for a virialized broad-line region (BLR). The velocity dispersion σ _line follows a similar trend in Types 1.5–1.8 but displays a sharp increase in Types 1.0–1.2, resulting in a dramatic drop in FWHM/ σ _line . These findings suggest that a virialized BLR together with accretion-dependent turbulent motions might be responsible for the diversity of BLR phenomena across the AGN population.https://doi.org/10.3847/1538-4365/ad9a5aActive galactic nucleiSupermassive black holesAccretionTime domain astronomyReverberation mapping |
| spellingShingle | Kai-Xing Lu Yan-Rong Li Qingwen Wu Luis C. Ho Zhi-Xiang Zhang Hai-Cheng Feng Sha-Sha Li Yong-Jie Chen Mouyuan Sun Xinwen Shu Wei-Jian Guo Cheng Cheng Jian-Guo Wang Dongchan Kim Jian-Min Wang Jin-Ming Bai A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 The Astrophysical Journal Supplement Series Active galactic nuclei Supermassive black holes Accretion Time domain astronomy Reverberation mapping |
| title | A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 |
| title_full | A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 |
| title_fullStr | A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 |
| title_full_unstemmed | A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 |
| title_short | A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018 |
| title_sort | short lived rejuvenation during the decades long changing look transition in the nucleus of mrk 1018 |
| topic | Active galactic nuclei Supermassive black holes Accretion Time domain astronomy Reverberation mapping |
| url | https://doi.org/10.3847/1538-4365/ad9a5a |
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