Properties of a Fading AGN from SDSS-IV MaNGA
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| Main Authors: | , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866914714403995648 |
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| author | Mo, Hao Chen, Yan-Mei Zhang, Zhi-Yun Moiseev, Alexei Bizyaev, Dmitry Shi, Yong Gu, Qiu-Sheng Bao, Min Cao, Xiao Li, Song-Lin |
| author_facet | Mo, Hao Chen, Yan-Mei Zhang, Zhi-Yun Moiseev, Alexei Bizyaev, Dmitry Shi, Yong Gu, Qiu-Sheng Bao, Min Cao, Xiao Li, Song-Lin |
| contents | We identify a fading AGN SDSS J220141.64+115124.3 from the internal Product Launch-11 (MPL-11) in Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The central region with a projected radius of $\sim$2.4 kpc is characterized as LINER-like line ratios while the outskirts extended to $\sim$15 kpc show Seyfert-like line ratios. The [OIII]$λ$5007 luminosity of the Seyfert regions is a factor of 37 (2) higher than the LINER regions without (with) dust attenuation correction, suggesting that the AGN activity decreases at least $\sim$8 $\times$ 10$^3$ yrs ($\sim$2.4 kpc/light-speed) ago. We model the emission line spectra in the central region with double Gaussian components (a narrow core and a broad wing) and analyze the properties of each component. The narrow core component mostly co-rotates with the stellar disc, whereas the broad wing component with a median of the velocity dispersion $\sim$300 km s$^{-1}$ is related to a wind outflow. The kinematic position angle (PA) of the ionized gas shows a $\sim$20° twist from the galaxy center to 1.5 effective radius. The median of the PA difference between the gas and stellar components is as large as $\sim$50° within 0.4 effective radius. The tidal feature in DESI image and star-gas misalignment suggest this galaxy is a merger remnant. Combining all these observational results as well as public available X-ray and MIR luminosities, we confirm this is a fading AGN, the merger process kick-started the central engine to quasar phase which ionized gas composed of tidal debris, and now the activity of the central black hole decreases. The discontinuity in [OIII]$λ$5007 flux and EQW maps is due to multiple AGN outbursts triggered by merger remnant gas inflows. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2403_09174 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Properties of a Fading AGN from SDSS-IV MaNGA Mo, Hao Chen, Yan-Mei Zhang, Zhi-Yun Moiseev, Alexei Bizyaev, Dmitry Shi, Yong Gu, Qiu-Sheng Bao, Min Cao, Xiao Li, Song-Lin Astrophysics of Galaxies We identify a fading AGN SDSS J220141.64+115124.3 from the internal Product Launch-11 (MPL-11) in Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The central region with a projected radius of $\sim$2.4 kpc is characterized as LINER-like line ratios while the outskirts extended to $\sim$15 kpc show Seyfert-like line ratios. The [OIII]$λ$5007 luminosity of the Seyfert regions is a factor of 37 (2) higher than the LINER regions without (with) dust attenuation correction, suggesting that the AGN activity decreases at least $\sim$8 $\times$ 10$^3$ yrs ($\sim$2.4 kpc/light-speed) ago. We model the emission line spectra in the central region with double Gaussian components (a narrow core and a broad wing) and analyze the properties of each component. The narrow core component mostly co-rotates with the stellar disc, whereas the broad wing component with a median of the velocity dispersion $\sim$300 km s$^{-1}$ is related to a wind outflow. The kinematic position angle (PA) of the ionized gas shows a $\sim$20° twist from the galaxy center to 1.5 effective radius. The median of the PA difference between the gas and stellar components is as large as $\sim$50° within 0.4 effective radius. The tidal feature in DESI image and star-gas misalignment suggest this galaxy is a merger remnant. Combining all these observational results as well as public available X-ray and MIR luminosities, we confirm this is a fading AGN, the merger process kick-started the central engine to quasar phase which ionized gas composed of tidal debris, and now the activity of the central black hole decreases. The discontinuity in [OIII]$λ$5007 flux and EQW maps is due to multiple AGN outbursts triggered by merger remnant gas inflows. |
| title | Properties of a Fading AGN from SDSS-IV MaNGA |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2403.09174 |