Circumnuclear Multi-phase Gas in the Circinus Galaxy. I. Non-LTE Calculations of CO Lines

Wada, Keiichi; Fukushige, Ryosuke; Izumi, Teruo; Tomisaka, Kohji

doi:10.3847/1538-4357/aa9e53

Cited by 43 publications

(42 citation statements)

References 52 publications

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“…Wada et al (2016) applied this radiation-driven fountain model to the Circinus galaxy, which is one of the closest (4.2 Mpc: Freeman et al 1977) type-2 AGN. The model is consistent with several observed features, such as the infrared spectral energy distribution (SED, Wada et al 2016), the dynamics of atomic/molecular gas (Wada et al 2018a;Izumi et al 2018;Uzuo et al 2021), distribution of ionized gas in the NLR (Wada et al 2018b), and broadband X-ray spectra (Buchner et al 2021). Mizumoto et al (2019) also suggested that this kind of dust driven wind may play an important role to the warm absorber acceleration.…”

Section: Introductionsupporting

confidence: 83%

Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei

Ogawa,

Ueda,

Wada

et al. 2021

Preprint

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To investigate the origins of the warm absorbers in active galactic nuclei (AGNs), we study the ionizationstate 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 (ξ) at a low inclination spreads over 4 orders of magnitude in ξ, 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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Section: Introductionsupporting

confidence: 83%

Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei

Ogawa,

Ueda,

Wada

et al. 2021

Preprint

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“…The dust particles in the central r < r sub ∼ 0.1-a few parsecs are sublimated owing to the heating by the central radiation. The radiation forms conical ionized gas (Narrow emission-line region) and also contributes to producing outflows of the dusty gas and torus (Wada 2012;Wada et al 2018;Izumi et al 2018). In the mid-plane of the torus, cold, dense gas forms a thin disk, where icy dust particles can present beyond the snow-line r snow .…”

Section: Introductionmentioning

confidence: 99%

Planet Formation around Supermassive Black Holes in the Active Galactic Nuclei

Wada

Tsukamoto

Kokubo

2019

ApJ

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As a natural consequence of the elementary processes of dust growth, we discovered that a new class of planets can be formed around supermassive black holes (SMBHs). We investigated a growth path from sub-micron sized icy dust monomers to Earthsized bodies outside the "snow line", located several parsecs from SMBHs in low luminosity active galactic nuclei (AGNs). In contrast to protoplanetary disks, the "radial drift barrier" does not prevent the formation of planetesimals. In the early phase of the evolution, low collision velocity between dust particles promotes sticking; therefore, the internal density of the dust aggregates decreases with growth. When the porous aggregate's size reaches 0.1-1 cm, the collisional compression becomes effective, and the decrease in internal density stops. Once 10-100 m sized aggregates are formed, they are decoupled from gas turbulence, and the aggregate layer becomes gravitationally unstable, leading to the formation of planets by the fragmentation of the layer, with ten times the mass of the earth. The growth time scale depends on the turbulent strength of the circumnuclear disk and the black hole mass M BH , and it is comparable to the AGN's lifetime (∼ 10 8 yr) for low mass (M BH ∼ 10 6 M ) SMBHs.

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“…(2016) geometry from their final simulation time step. Figure 1 shows the geometry for a black hole mass of M BH = 2 × 10 6 M and 20% Eddington rate, suitable for comparison to Circinus (see Wada et al 2016Wada et al , 2018aIzumi et al 2018;Wada et al 2018b, for comparison with infrared SEDs, atomic/molecular gas, and ionized gas observations, respectively). The model has a Compton-thick LOS column density only under edgeon viewing angles (consistent with the infrared analysis of Circinus by Wada et al 2016).…”

Section: Wada's Radiative Fountain Modelmentioning

confidence: 99%

Physically motivated X-ray obscurer models

Buchner,

Brightman,

Baloković

et al. 2021

Preprint

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Context. The nuclear obscurer of Active Galactic Nuclei (AGN) is poorly understood in terms of its origin, geometry and dynamics. Aims. We investigate whether physically motivated geometries emerging from hydro-radiative simulations can be differentiated with X-ray reflection spectroscopy. Methods. For two new geometries, the radiative fountain model of Wada ( 2012) and a warped disk, we release spectral models produced with the ray tracing code XARS. We contrast these models with spectra of three nearby AGN taken by NuSTAR and Swift/BAT. Results. Along heavily obscured sight-lines, the models present different 4-20 keV continuum spectra. These can be differentiated by current observations. Spectral fits of the Circinus Galaxy favor the warped disk model over the radiative fountain, and clumpy or smooth torus models. Conclusions. The necessary reflector (NH ≥ 10 25 cm 2 ) suggests a hidden population of heavily Compton-thick AGN amongst local galaxies. X-ray reflection spectroscopy is a promising pathway to understand the nuclear obscurer in AGN.

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Circumnuclear Multi-phase Gas in the Circinus Galaxy. I. Non-LTE Calculations of CO Lines

Cited by 43 publications

References 52 publications

Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei

Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei

Planet Formation around Supermassive Black Holes in the Active Galactic Nuclei

Physically motivated X-ray obscurer models

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