The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
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arXiv
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| Autori principali: | , , , , , , |
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| Natura: | Preprint |
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2024
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| author | Li, Ruancun Ricci, Claudio Ho, Luis C. Trakhtenbrot, Benny Kara, Erin Masterson, Megan Arcavi, Iair |
| author_facet | Li, Ruancun Ricci, Claudio Ho, Luis C. Trakhtenbrot, Benny Kara, Erin Masterson, Megan Arcavi, Iair |
| contents | Time-domain studies of active galactic nuclei (AGNs) offer a powerful tool for understanding black hole accretion physics. Prior to the optical outburst on 23 December 2017, 1ES 1927+654 was classified as a "true" type~2 AGN, an unobscured source intrinsically devoid of broad-line emission in polarized spectra. Through our three-year monitoring campaign spanning X-ray to ultraviolet/optical wavelengths, we analyze the post-outburst evolution of the spectral energy distribution (SED) of 1ES 1927+654. Examination of the intrinsic SED and subsequent modeling using different models reveal that the post-outburst spectrum is best described by a combination of a disk, blackbody, and corona components. We detect systematic SED variability and identify four distinct stages in the evolution of these components. During the event the accretion rate is typically above the Eddington limit. The correlation between ultraviolet luminosity and optical to X-ray slope ($α_\mathrm{OX}$) resembles that seen in previous studies of type 1 AGNs, yet exhibits two distinct branches with opposite slopes. The optical bolometric correction factor ($κ_{5100}$) is $\sim 10$ times higher than typical AGNs, again displaying two distinct branches. Correlations among the corona optical depth, disk surface density, and $α_\mathrm{OX}$ provide compelling evidence of a disk-corona connection. The X-ray corona showcases systematic variation in the compactness-temperature plot. Between 200 and 650 days, the corona is "hotter-when-brighter", whereas after 650 days, it becomes "cooler-when-brighter". This bimodal behavior, in conjunction with the bifurcated branches of $α_\mathrm{OX}$ and $κ_{5100}$, offers strong evidence of a transition from a slim disk to thin disk $\sim 650$ days after the outburst. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_09264 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654 Li, Ruancun Ricci, Claudio Ho, Luis C. Trakhtenbrot, Benny Kara, Erin Masterson, Megan Arcavi, Iair High Energy Astrophysical Phenomena Time-domain studies of active galactic nuclei (AGNs) offer a powerful tool for understanding black hole accretion physics. Prior to the optical outburst on 23 December 2017, 1ES 1927+654 was classified as a "true" type~2 AGN, an unobscured source intrinsically devoid of broad-line emission in polarized spectra. Through our three-year monitoring campaign spanning X-ray to ultraviolet/optical wavelengths, we analyze the post-outburst evolution of the spectral energy distribution (SED) of 1ES 1927+654. Examination of the intrinsic SED and subsequent modeling using different models reveal that the post-outburst spectrum is best described by a combination of a disk, blackbody, and corona components. We detect systematic SED variability and identify four distinct stages in the evolution of these components. During the event the accretion rate is typically above the Eddington limit. The correlation between ultraviolet luminosity and optical to X-ray slope ($α_\mathrm{OX}$) resembles that seen in previous studies of type 1 AGNs, yet exhibits two distinct branches with opposite slopes. The optical bolometric correction factor ($κ_{5100}$) is $\sim 10$ times higher than typical AGNs, again displaying two distinct branches. Correlations among the corona optical depth, disk surface density, and $α_\mathrm{OX}$ provide compelling evidence of a disk-corona connection. The X-ray corona showcases systematic variation in the compactness-temperature plot. Between 200 and 650 days, the corona is "hotter-when-brighter", whereas after 650 days, it becomes "cooler-when-brighter". This bimodal behavior, in conjunction with the bifurcated branches of $α_\mathrm{OX}$ and $κ_{5100}$, offers strong evidence of a transition from a slim disk to thin disk $\sim 650$ days after the outburst. |
| title | The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2409.09264 |