Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release
We present the identification of changing-look active galactic nuclei (CL-AGNs) from the Dark Energy Spectroscopic Instrument First Data Release and Sloan Digital Sky Survey Data Release 16 at z ≤ 0.9. To confirm the CL-AGNs, we utilize spectral flux calibration assessment via an [O iii ]-based cali...
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2025-01-01
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| author | Wei-Jian Guo Hu Zou Claire L. Greenwell David M. Alexander Victoria A. Fawcett Zhiwei Pan Małgorzata Siudek Jessica Nicole Aguilar Steven Ahlen David Brooks Todd Claybaugh Kyle Dawson Axel de la Macorra Peter Doel Andreu Font-Ribera Enrique Gaztañaga Satya Gontcho A Gontcho Gaston Gutierrez Robert Kehoe Theodore Kisner Martin Landriau Laurent Le Guillou Marc Manera Aaron Meisner Ramon Miquel John Moustakas Francisco Prada Graziano Rossi Eusebio Sanchez Michael Schubnell David Sprayberry Jipeng Sui Gregory Tarlé Benjamin Alan Weaver Yun-Ao Xiao Siwei Zou |
| author_facet | Wei-Jian Guo Hu Zou Claire L. Greenwell David M. Alexander Victoria A. Fawcett Zhiwei Pan Małgorzata Siudek Jessica Nicole Aguilar Steven Ahlen David Brooks Todd Claybaugh Kyle Dawson Axel de la Macorra Peter Doel Andreu Font-Ribera Enrique Gaztañaga Satya Gontcho A Gontcho Gaston Gutierrez Robert Kehoe Theodore Kisner Martin Landriau Laurent Le Guillou Marc Manera Aaron Meisner Ramon Miquel John Moustakas Francisco Prada Graziano Rossi Eusebio Sanchez Michael Schubnell David Sprayberry Jipeng Sui Gregory Tarlé Benjamin Alan Weaver Yun-Ao Xiao Siwei Zou |
| author_sort | Wei-Jian Guo |
| collection | DOAJ |
| description | We present the identification of changing-look active galactic nuclei (CL-AGNs) from the Dark Energy Spectroscopic Instrument First Data Release and Sloan Digital Sky Survey Data Release 16 at z ≤ 0.9. To confirm the CL-AGNs, we utilize spectral flux calibration assessment via an [O iii ]-based calibration, pseudophotometry examination, and visual inspection. This rigorous selection process allows us to compile a statistical catalog of 561 CL-AGNs, encompassing 527 H β , 149 H α , and 129 Mg ii CL behaviors. In this sample, we find (1) a 283:278 ratio of turn-on to turn-off CL-AGNs. (2) The median Eddington ratio for CL-AGNs in the dim state is approximately λ _Edd ∼ 0.01. (3) A strong correlation between the change in the luminosity of the broad emission lines (BELs) and variation in the continuum luminosity, with Mg ii and H β displaying similar responses during CL phases. (4) The Baldwin–Phillips–Terlevich diagram for CL-AGNs shows no statistical difference from the general AGN catalog. (5) Five CL-AGNs are associated with asymmetrical mid-infrared flares, possibly linked to tidal disruption events. Given the large CL-AGN sample and the stochastic sampling of spectra, we propose that some CL phenomena are inherently due to typical AGN variability during low accretion rates, particularly for CL phenomenon only occurring on one BEL. Finally, we introduce a monotonically dimming CL phase for objects characterized by a gradual decline over decades in the light curve and the complete disappearance of entire BELs in faint spectra, indicative of a real transition in the accretion disk. |
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| institution | Kabale University |
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| spelling | doaj-art-79967c99ed594b27bb65d9f8a4d0cc852025-08-20T03:52:14ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127812810.3847/1538-4365/adc124Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data ReleaseWei-Jian Guo0https://orcid.org/0000-0001-9457-0589Hu Zou1https://orcid.org/0000-0002-6684-3997Claire L. Greenwell2https://orcid.org/0000-0002-7719-5809David M. Alexander3https://orcid.org/0000-0002-5896-6313Victoria A. Fawcett4https://orcid.org/0000-0003-1251-532XZhiwei Pan5https://orcid.org/0000-0003-0230-6436Małgorzata Siudek6https://orcid.org/0000-0002-2949-2155Jessica Nicole Aguilar7Steven Ahlen8https://orcid.org/0000-0001-6098-7247David Brooks9https://orcid.org/0000-0002-8458-5047Todd Claybaugh10Kyle Dawson11Axel de la Macorra12https://orcid.org/0000-0002-1769-1640Peter Doel13https://orcid.org/0000-0002-6397-4457Andreu Font-Ribera14https://orcid.org/0000-0002-3033-7312Enrique Gaztañaga15Satya Gontcho A Gontcho16https://orcid.org/0000-0003-3142-233XGaston Gutierrez17Robert Kehoe18https://orcid.org/0000-0002-7101-697XTheodore Kisner19https://orcid.org/0000-0003-3510-7134Martin Landriau20https://orcid.org/0000-0003-1838-8528Laurent Le Guillou21https://orcid.org/0000-0001-7178-8868Marc Manera22https://orcid.org/0000-0003-4962-8934Aaron Meisner23https://orcid.org/0000-0002-1125-7384Ramon Miquel24John Moustakas25https://orcid.org/0000-0002-2733-4559Francisco Prada26https://orcid.org/0000-0001-7145-8674Graziano Rossi27Eusebio Sanchez28https://orcid.org/0000-0002-9646-8198Michael Schubnell29David Sprayberry30https://orcid.org/0000-0001-7583-6441Jipeng Sui31Gregory Tarlé32https://orcid.org/0000-0003-1704-0781Benjamin Alan Weaver33Yun-Ao Xiao34https://orcid.org/0009-0004-2243-8289Siwei Zou35https://orcid.org/0000-0002-3983-6484Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China ; guowj@bao.ac.cnNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100012, People’s Republic of China ; zouhu@bao.ac.cnInstitute for Computational Cosmology, Department of Physics, Durham University , South Road, Durham DH1 3LE, UKInstitute for Computational Cosmology, Department of Physics, Durham University , South Road, Durham DH1 3LE, UK; Centre for Extragalactic Astronomy, Department of Physics, Durham University , South Road, Durham, DH1 3LE, UKSchool of Mathematics, Statistics and Physics, Newcastle University , Newcastle upon Tyne, NE1 7RU, UKKavli Institute for Astronomy and Astrophysics at Peking University , PKU, 5 Yiheyuan Road, Haidian District, Beijing 100871, People’s Republic of ChinaInstitute of Space Sciences , ICE-CSIC, Campus UAB, Carrer de Can Magrans s/n, 08913 Bellaterra, Barcelona, SpainLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USAPhysics Dept., Boston University , 590 Commonwealth Avenue, Boston, MA 02215, USADepartment of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UKLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USADepartment of Physics and Astronomy, The University of Utah , 115 South 1400 East, Salt Lake City, UT 84112, USAInstituto de Física, Universidad Nacional Autónoma de México , Cd. de México C.P. 04510, MexicoDepartment of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UKDepartment of Physics & Astronomy, University College London , Gower Street, London, WC1E 6BT, UK; Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, 08193 Bellaterra, Barcelona, SpainInstitute of Space Sciences , ICE-CSIC, Campus UAB, Carrer de Can Magrans s/n, 08913 Bellaterra, Barcelona, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , 08034 Barcelona, Spain; Institute of Cosmology and Gravitation, University of Portsmouth , Dennis Sciama Building, Portsmouth, PO1 3FX, UKLawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USAFermi National Accelerator Laboratory , PO Box 500, Batavia, IL 60510, USADepartment of Physics, Southern Methodist University , 3215 Daniel Avenue, Dallas, TX 75275, USALawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USALawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720, USASorbonne Université , CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), FR-75005 Paris, FranceInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, 08193 Bellaterra, Barcelona, Spain; Departament de Física, Serra Húnter, Universitat Autònoma de Barcelona , 08193 Bellaterra (Barcelona), SpainNSF NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USAInstitut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, 08193 Bellaterra, Barcelona, Spain; Institució Catalana de Recerca i Estudis Avançats , Passeig de Lluís Companys, 23, 08010 Barcelona, SpainDepartment of Physics and Astronomy, Siena College , 515 Loudon Road, Loudonville, NY 12211, USAInstituto de Astrofísica de Andalucía (CSIC) , Glorieta de la Astronomía, s/n, E-18008 Granada, SpainDepartment of Physics and Astronomy, Sejong University , Seoul, 143-747, Republic of KoreaCIEMAT , Avenida Complutense 40, E-28040 Madrid, SpainDepartment of Physics, University of Michigan , Ann Arbor, MI 48109, USA; University of Michigan , Ann Arbor, MI 48109, USANSF NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USANational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100012, People’s Republic of China ; zouhu@bao.ac.cnUniversity of Michigan , Ann Arbor, MI 48109, USANSF NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USANational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100012, People’s Republic of China ; zouhu@bao.ac.cnChinese Academy of Sciences South America Center for Astronomy , National Astronomical Observatories, CAS, Beijing 100101, People’s Republic of China; Department of Astronomy, Tsinghua University , Beijing 100084, People’s Republic of ChinaWe present the identification of changing-look active galactic nuclei (CL-AGNs) from the Dark Energy Spectroscopic Instrument First Data Release and Sloan Digital Sky Survey Data Release 16 at z ≤ 0.9. To confirm the CL-AGNs, we utilize spectral flux calibration assessment via an [O iii ]-based calibration, pseudophotometry examination, and visual inspection. This rigorous selection process allows us to compile a statistical catalog of 561 CL-AGNs, encompassing 527 H β , 149 H α , and 129 Mg ii CL behaviors. In this sample, we find (1) a 283:278 ratio of turn-on to turn-off CL-AGNs. (2) The median Eddington ratio for CL-AGNs in the dim state is approximately λ _Edd ∼ 0.01. (3) A strong correlation between the change in the luminosity of the broad emission lines (BELs) and variation in the continuum luminosity, with Mg ii and H β displaying similar responses during CL phases. (4) The Baldwin–Phillips–Terlevich diagram for CL-AGNs shows no statistical difference from the general AGN catalog. (5) Five CL-AGNs are associated with asymmetrical mid-infrared flares, possibly linked to tidal disruption events. Given the large CL-AGN sample and the stochastic sampling of spectra, we propose that some CL phenomena are inherently due to typical AGN variability during low accretion rates, particularly for CL phenomenon only occurring on one BEL. Finally, we introduce a monotonically dimming CL phase for objects characterized by a gradual decline over decades in the light curve and the complete disappearance of entire BELs in faint spectra, indicative of a real transition in the accretion disk.https://doi.org/10.3847/1538-4365/adc124Active galactic nucleiActive galaxiesAccretionSupermassive black holesCatalogs |
| spellingShingle | Wei-Jian Guo Hu Zou Claire L. Greenwell David M. Alexander Victoria A. Fawcett Zhiwei Pan Małgorzata Siudek Jessica Nicole Aguilar Steven Ahlen David Brooks Todd Claybaugh Kyle Dawson Axel de la Macorra Peter Doel Andreu Font-Ribera Enrique Gaztañaga Satya Gontcho A Gontcho Gaston Gutierrez Robert Kehoe Theodore Kisner Martin Landriau Laurent Le Guillou Marc Manera Aaron Meisner Ramon Miquel John Moustakas Francisco Prada Graziano Rossi Eusebio Sanchez Michael Schubnell David Sprayberry Jipeng Sui Gregory Tarlé Benjamin Alan Weaver Yun-Ao Xiao Siwei Zou Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release The Astrophysical Journal Supplement Series Active galactic nuclei Active galaxies Accretion Supermassive black holes Catalogs |
| title | Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release |
| title_full | Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release |
| title_fullStr | Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release |
| title_full_unstemmed | Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release |
| title_short | Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. II. Statistical Properties from the First Data Release |
| title_sort | changing look active galactic nuclei from the dark energy spectroscopic instrument ii statistical properties from the first data release |
| topic | Active galactic nuclei Active galaxies Accretion Supermassive black holes Catalogs |
| url | https://doi.org/10.3847/1538-4365/adc124 |
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