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Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei
High Energy Astrophysical Phenomena · Submitted 30 Nov 2021
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These results suggest that the ionized gas launched from sub-parsec or smaller regions inside the torus, which are not included in the current fountain model, must be important ingredients of the warm absorbers with a few thousands km s$^{-1}$.
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To investigate the origins of the warm absorbers in active galactic nuclei (AGNs), we study the ionization-state structure of the radiation-driven fountain model in a low-mass AGN (Wada et al. 2016) and calculate the predicted X-ray spectra, utilizing the spectral synthesis code Cloudy (Ferland et al. 2017). The spectra show many absorption and emission line features originated in the outflowing ionized gas. The O VIII 0.654 keV lines are produced mainly in the polar region much closer to the SMBH than the optical narrow line regions. The absorption measure distribution of the ionization parameter ($\xi$) at a low inclination spreads over 4 orders of magnitude in $\xi$, indicating multi-phase ionization structure of the outflow, as actually observed in many type-1 AGNs. We compare our simulated spectra with the high energy-resolution spectrum of the narrow line Seyfert 1 galaxy, NGC 4051. The model reproduces slowly outflowing (a few hundreds km s$^{-1}$) warm absorbers. However, the faster components with a few thousands km s$^{-1}$ observed in NGC 4051 are not reproduced. The simulation also underproduces the intensity and width of the O VIII 0.654 keV line. These results suggest that the ionized gas launched from sub-parsec or smaller regions inside the torus, which are not included in the current fountain model, must be important ingredients of the warm absorbers with a few thousands km s$^{-1}$. The model also consistently explains the Chandra/HETG spectrum of the Seyfert 2 galaxy, the Circinus galaxy.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | To investigate the origins of the warm absorbers in active galactic nuclei (AGNs), we study the ionization-state structure of the radiation-driven fountain model in a low-mass AGN (Wada et al. 2016) and calculate the predicted X-ray spectra, utilizing the spectral synthesis code Cloudy (Ferland et al. 2017). | contribution 0.60 | 0.89 | 0.04 | asserted 0.84 |
| s1 | The spectra show many absorption and emission line features originated in the outflowing ionized gas. | result 1.00 | 0.87 | 0.04 | asserted 1.00 |
| s2 | The O VIII 0.654 keV lines are produced mainly in the polar region much closer to the SMBH than the optical narrow line regions. | result 1.00 | 0.86 | 0.06 | asserted 1.00 |
| s3 | The absorption measure distribution of the ionization parameter ($\xi$) at a low inclination spreads over 4 orders of magnitude in $\xi$, indicating multi-phase ionization structure of the outflow, as actually observed in many type-1 AGNs. | result 0.95 | 0.86 | 0.10 | hedged possibility 0.66 |
| s4 | We compare our simulated spectra with the high energy-resolution spectrum of the narrow line Seyfert 1 galaxy, NGC 4051. | method 0.76 | 0.87 | 0.03 | asserted 0.97 |
| s5 | The model reproduces slowly outflowing (a few hundreds km s$^{-1}$) warm absorbers. | result 1.00 | 0.89 | 0.10 | asserted 1.00 |
| s6 | However, the faster components with a few thousands km s$^{-1}$ observed in NGC 4051 are not reproduced. | limitation 0.81 | 0.86 | 0.11 | asserted 1.00 |
| s7 | The simulation also underproduces the intensity and width of the O VIII 0.654 keV line. | limitation 0.59 | 0.91 | 0.07 | asserted 1.00 |
| s8 | These results suggest that the ionized gas launched from sub-parsec or smaller regions inside the torus, which are not included in the current fountain model, must be important ingredients of the warm absorbers with a few thousands km s$^{-1}$. | interpretation 1.00 | 0.72 | 0.76 | hedged possibility 1.00 |
| s9 | The model also consistently explains the Chandra/HETG spectrum of the Seyfert 2 galaxy, the Circinus galaxy. | result 1.00 | 0.87 | 0.08 | asserted 0.90 |
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Original abstract
To investigate the origins of the warm absorbers in active galactic nuclei (AGNs), we study the ionization-state structure of the radiation-driven fountain model in a low-mass AGN (Wada et al. 2016) and calculate the predicted X-ray spectra, utilizing the spectral synthesis code Cloudy (Ferland et al. 2017). The spectra show many absorption and emission line features originated in the outflowing ionized gas. The O VIII 0.654 keV lines are produced mainly in the polar region much closer to the SMBH than the optical narrow line regions. The absorption measure distribution of the ionization parameter ($\xi$) at a low inclination spreads over 4 orders of magnitude in $\xi$, indicating multi-phase ionization structure of the outflow, as actually observed in many type-1 AGNs. We compare our simulated spectra with the high energy-resolution spectrum of the narrow line Seyfert 1 galaxy, NGC 4051. The model reproduces slowly outflowing (a few hundreds km s$^{-1}$) warm absorbers. However, the faster components with a few thousands km s$^{-1}$ observed in NGC 4051 are not reproduced. The simulation also underproduces the intensity and width of the O VIII 0.654 keV line. These results suggest that the ionized gas launched from sub-parsec or smaller regions inside the torus, which are not included in the current fountain model, must be important ingredients of the warm absorbers with a few thousands km s$^{-1}$. The model also consistently explains the Chandra/HETG spectrum of the Seyfert 2 galaxy, the Circinus galaxy.
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They constitute essential elements of the AGN structure, such as jets, warm absorbers, narrow emission line regions (NLRs), and tori [ref] .
The Galaxy Activity, Torus and Outflow Survey (GATOS): II. Torus and polar dust emission in nearby Seyfert galaxies · Introduction · 0.96
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