Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142
We performed a rigorous reverberation-mapping analysis of the broad-line region (BLR) in a highly accreting ( L / L _Edd = 0.74–3.4) active galactic nucleus, Markarian 142 (Mrk 142), for the first time using concurrent observations of the inner accretion disk and the BLR to determine a time lag for...
| Main Authors: | , , , , , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acfb72 |
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| author | Viraja C. Khatu Sarah C. Gallagher Keith Horne Edward M. Cackett Chen Hu Sofia Pasquini Patrick Hall Jian-Min Wang Wei-Hao Bian Yan-Rong Li Jin-Ming Bai Yong-Jie Chen Pu Du Michael Goad Bo-Wei Jiang Sha-Sha Li Yu-Yang Songsheng Chan Wang Ming Xiao Zhe Yu |
| author_facet | Viraja C. Khatu Sarah C. Gallagher Keith Horne Edward M. Cackett Chen Hu Sofia Pasquini Patrick Hall Jian-Min Wang Wei-Hao Bian Yan-Rong Li Jin-Ming Bai Yong-Jie Chen Pu Du Michael Goad Bo-Wei Jiang Sha-Sha Li Yu-Yang Songsheng Chan Wang Ming Xiao Zhe Yu |
| author_sort | Viraja C. Khatu |
| collection | DOAJ |
| description | We performed a rigorous reverberation-mapping analysis of the broad-line region (BLR) in a highly accreting ( L / L _Edd = 0.74–3.4) active galactic nucleus, Markarian 142 (Mrk 142), for the first time using concurrent observations of the inner accretion disk and the BLR to determine a time lag for the H β λ 4861 emission relative to the ultraviolet (UV) continuum variations. We used continuum data taken with the Niel Gehrels Swift Observatory in the UVW 2 band, and the Las Cumbres Observatory, Dan Zowada Memorial Observatory, and Liverpool Telescope in the g band, as part of the broader Mrk 142 multiwavelength monitoring campaign in 2019. We obtained new spectroscopic observations covering the H β broad emission line in the optical from the Gemini North Telescope and the Lijiang 2.4 m Telescope for a total of 102 epochs (over a period of 8 months) contemporaneous to the continuum data. Our primary result states a UV-to-H β time lag of ${8.68}_{-0.72}^{+0.75}$ days in Mrk 142 obtained from light-curve analysis with a Python-based running optimal average algorithm. We placed our new measurements for Mrk 142 on the optical and UV radius–luminosity relations for NGC 5548 to understand the nature of the continuum driver. The positions of Mrk 142 on the scaling relations suggest that UV is closer to the “true” driving continuum than the optical. Furthermore, we obtain $\mathrm{log}({M}_{\bullet }/{M}_{\odot })$ = 6.32 ± 0.29 assuming UV as the primary driving continuum. |
| first_indexed | 2024-03-11T06:59:58Z |
| format | Article |
| id | doaj.art-d61ac719e05840c7b7bf6d17d557151e |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T06:59:58Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-d61ac719e05840c7b7bf6d17d557151e2023-11-17T09:21:04ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01958212710.3847/1538-4357/acfb72Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142Viraja C. Khatu0https://orcid.org/0000-0002-0581-6506Sarah C. Gallagher1https://orcid.org/0000-0001-6217-8101Keith Horne2https://orcid.org/0000-0003-1728-0304Edward M. Cackett3https://orcid.org/0000-0002-8294-9281Chen Hu4Sofia Pasquini5Patrick Hall6https://orcid.org/0000-0002-1763-5825Jian-Min Wang7https://orcid.org/0000-0001-9449-9268Wei-Hao Bian8https://orcid.org/0000-0002-2121-8960Yan-Rong Li9https://orcid.org/0000-0001-5841-9179Jin-Ming Bai10Yong-Jie Chen11Pu Du12https://orcid.org/0000-0002-5830-3544Michael Goad13Bo-Wei Jiang14https://orcid.org/0000-0003-3825-0710Sha-Sha Li15https://orcid.org/0000-0003-3823-3419Yu-Yang Songsheng16https://orcid.org/0000-0003-4042-7191Chan Wang17Ming Xiao18https://orcid.org/0000-0001-5981-6440Zhe Yu19Department of Physics and Astronomy & Institute of Earth and Space Exploration, The University of Western Ontario , 1151 Richmond Street, London, Ontario N6A 3K7, Canada ; vkhatu@uwo.caDepartment of Physics and Astronomy & Institute of Earth and Space Exploration, The University of Western Ontario , 1151 Richmond Street, London, Ontario N6A 3K7, Canada ; vkhatu@uwo.caSchool of Physics and Astronomy, University of St Andrews , North Haugh, St Andrews, KY16 9SS, Scotland, UKDepartment of Physics & Astronomy, Wayne State University , 666 W Hancock Street, Detroit, MI 48201, USAKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People's Republic of ChinaDepartment of Physics and Astronomy, The University of Western Ontario , 1151 Richmond Street, London, Ontario N6A 3K7, CanadaDepartment of Physics and Astronomy, York University , 4700 Keele Street, Toronto, Ontario M3J 1P3, CanadaKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People's Republic of ChinaPhysics Department, Nanjing Normal University , Nanjing 210097, 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 ChinaYunnan Observatories, The 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 ChinaKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People's Republic of ChinaSchool of Physics and Astronomy, University of Leicester , Leicester LE1 7RH, UKKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People's Republic of ChinaYunnan Observatories, The 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 ChinaPhysics Department, Nanjing Normal University , Nanjing 210097, 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 ChinaKey Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences , 19B Yuquan Road, Beijing 100049, People's Republic of ChinaWe performed a rigorous reverberation-mapping analysis of the broad-line region (BLR) in a highly accreting ( L / L _Edd = 0.74–3.4) active galactic nucleus, Markarian 142 (Mrk 142), for the first time using concurrent observations of the inner accretion disk and the BLR to determine a time lag for the H β λ 4861 emission relative to the ultraviolet (UV) continuum variations. We used continuum data taken with the Niel Gehrels Swift Observatory in the UVW 2 band, and the Las Cumbres Observatory, Dan Zowada Memorial Observatory, and Liverpool Telescope in the g band, as part of the broader Mrk 142 multiwavelength monitoring campaign in 2019. We obtained new spectroscopic observations covering the H β broad emission line in the optical from the Gemini North Telescope and the Lijiang 2.4 m Telescope for a total of 102 epochs (over a period of 8 months) contemporaneous to the continuum data. Our primary result states a UV-to-H β time lag of ${8.68}_{-0.72}^{+0.75}$ days in Mrk 142 obtained from light-curve analysis with a Python-based running optimal average algorithm. We placed our new measurements for Mrk 142 on the optical and UV radius–luminosity relations for NGC 5548 to understand the nature of the continuum driver. The positions of Mrk 142 on the scaling relations suggest that UV is closer to the “true” driving continuum than the optical. Furthermore, we obtain $\mathrm{log}({M}_{\bullet }/{M}_{\odot })$ = 6.32 ± 0.29 assuming UV as the primary driving continuum.https://doi.org/10.3847/1538-4357/acfb72Active galactic nucleiAccretionSpectroscopy |
| spellingShingle | Viraja C. Khatu Sarah C. Gallagher Keith Horne Edward M. Cackett Chen Hu Sofia Pasquini Patrick Hall Jian-Min Wang Wei-Hao Bian Yan-Rong Li Jin-Ming Bai Yong-Jie Chen Pu Du Michael Goad Bo-Wei Jiang Sha-Sha Li Yu-Yang Songsheng Chan Wang Ming Xiao Zhe Yu Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 The Astrophysical Journal Active galactic nuclei Accretion Spectroscopy |
| title | Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 |
| title_full | Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 |
| title_fullStr | Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 |
| title_full_unstemmed | Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 |
| title_short | Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. XIII. Ultraviolet Time Lag of Hβ Emission in Mrk 142 |
| title_sort | supermassive black holes with high accretion rates in active galactic nuclei xiii ultraviolet time lag of hβ emission in mrk 142 |
| topic | Active galactic nuclei Accretion Spectroscopy |
| url | https://doi.org/10.3847/1538-4357/acfb72 |
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