論文 - 和田　桂一

Tanimoto, Atsushi ; Wada, Keiichi ; Odaka, Hirokazu ; Kudoh, Yuki ; Nozomu, Kawakatu .  X-Ray Radiative Transfer Calculation Based on a Physics-based Model of the Sub-parsec-scale Gases around an Active Galactic Nucleus and Its Application to NGC 3783 .  The Astrophysical Journal   2025年査読

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.48550/arXiv.2505.09693

Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura .  Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows .  The Astrophysical Journal977 ( 1 ) 48 - 48   2024年12月査読 国際共著 国際誌

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掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

We investigated the influence of the Eddington ratio on sub-parsec-scale outflows in active galactic nuclei (AGNs) with supermassive black holes (SMBHs) masses of 10⁷ M _⊙ using two-dimensional radiation hydrodynamics simulations. When the range of the Eddington ratio is γ _Edd > 10⁻³, the radiation force exceeds the gas pressure, leading to stronger outflows and larger dust sublimation radius. Although the sub-parsec-scale outflows are a time-dependent phenomenon, our simulations demonstrated that the radial distributions can be well explained by the steady solutions of the spherically symmetric stellar winds. The dynamic structure of sub-parsec-scale outflows is influenced by the dust sublimation radius and the critical radii determined by the dynamical equilibrium condition. Although significantly affecting the outflow velocity, the Eddington ratio exerts minimal effects on temperature and number density distribution. Furthermore, our analytical solutions highlight the importance of the dust sublimation scale as a crucial determinant of terminal velocity and column density in dusty outflows. Through comparisons of our numerical model with the obscuring fraction observed in nearby AGNs, we reveal insights into the Eddington ratio dependence and the tendency toward the large obscuring fraction of the dusty and dust-free gases. The analytical solutions are expected to facilitate an understanding of the dynamical structure and radiation structures along the line of sight and their viewing angles from observations of ionized outflows.

DOI： 10.3847/1538-4357/ad8b42

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ad8b42/pdf

Vander Meulen, Bert; Camps, Peter; Tsujimoto, Masahiro; Wada, Keiichi .  Intrinsic line profiles for X-ray fluorescent lines in SKIRT .  Astronomy & Astrophysics688   L33 - L38   2024年8月査読 国際共著

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1051/0004-6361/202451370

Shunsuke Baba, Keiichi Wada, Takuma Izumi, Yuki Kudoh, Kosei Matsumoto .  Circumnuclear Multiphase Gas in the Circinus Galaxy. VI. Detectability of Molecular Inflow and Atomic Outflow .  The Astrophysical Journal966 ( 1 ) 15   2024年5月査読 国際共著 国際誌

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記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：IOP Publishing  

Recent submillimeter observations have revealed signs of pc-scale molecular
inflow and atomic outflow in the nearest Seyfert 2 galaxy, the Circinus galaxy.
To verify the gas kinematics suggested by these observations, we performed
molecular and atomic line transfer calculations based on a physics-based 3D
radiation-hydrodynamic model, which has been compared with multi-wavelength
observations in this paper series. The major axis position-velocity diagram
(PVD) of CO(3-2) reproduces the observed faint emission at the systemic
velocity, and our calculations confirm that this component originates from
failed winds falling back to the disk plane. The minor-axis PVD of
[CI]($^3P_1$-$^3P_0$), when created using only the gas with positive radial
velocities, presents a sign of blue- and redshifted offset peaks similar to
those in the observation, suggesting that the observed peaks indeed originate
from the outflow, but that the model may lack outflows as strong as those in
the Circinus galaxy. Similar to the observed HCN(3-2), the similar dense gas
tracer HCO$^+$(3-2) can exhibit nuclear spectra with inverse P-Cygni profiles
with $\sim$0.5 pc beams, but the line shape is azimuthally dependent. The
corresponding continuum absorbers are inflowing clumps at 5-10 pc from the
center. To detect significant absorption with a high probability, the
inclination must be fairly edge-on ($\gtrsim$85$^\circ$), and the beam size
must be small ($\lesssim$1 pc). These results suggest that HCN or HCO$^+$ and
[CI] lines are effective for observing pc-scale inflows and outflows,
respectively.

DOI： 10.3847/1538-4357/ad34d3

arXiv

Satoshi Yamada, Yoshihiro Ueda, Taiki Kawamuro, Claudio Ricci, Yoshiki Toba, Masatoshi Imanishi, Takamitsu Miyaji, Atsushi Tanimoto, Kohei Ichikawa, Martín Herrera-Endoqui, Shoji Ogawa, Ryosuke Uematsu, Keiichi Wada .  [O iv]- and [Ne v]-weak Active Galactic Nuclei Hidden by Compton-thick Material in Late Mergers .  Astrophysical Journal965 ( 2 )   2024年4月

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掲載種別：研究論文（学術雑誌）  

We study “buried” active galactic nuclei (AGNs) almost fully covered by circumnuclear material in ultra/luminous infrared galaxies (U/LIRGs), which show weak ionized lines from narrow-line regions. Employing an indicator of a [O iv] 25.89 or [Ne v] 14.32 μm line to 12 μm AGN luminosity ratio, we find 17 buried AGN candidates that are [O iv]-weak (L [O IV]/L 12,AGN ≤ −3.0) or [Ne v]-weak (L [Ne V]/L 12,AGN ≤ −3.4) among 30 AGNs in local U/LIRGs. For the [O iv]-weak AGNs, we estimate their covering fractions of Compton-thick (CT; N H ≥ 1024 cm−2) material with an X-ray clumpy torus model to be f CT ( spec ) = 0.55 ± 0.19 on average. This value is consistent with the fraction of CT AGNs ( f CT ( stat ) = 53 % ± 12 % ) among the [O iv]-weak AGNs in U/LIRGs and much larger than that in Swift/Burst Alert Telescope (BAT) AGNs (23% ± 6%). The fraction of [O iv]-weak AGNs increases from 27 − 10 + 13 % (early) to 66 − 12 + 10 % (late mergers). Similar results are obtained with the [Ne v] line. The [O iv]- or [Ne v]-weak AGNs in late mergers show larger N H and Eddington ratios (λ Edd) than those of the Swift/BAT AGNs, and the largest N H is ≳1025 cm−2 at log λ Edd ∼ − 1 , close to the effective Eddington limit for CT material. These suggest that (1) the circumnuclear material in buried AGNs is regulated by the radiation force from high-λ Edd AGNs on the CT obscurers, and (2) their dense material with large f CT ( spec ) (∼0.5 ± 0.1) in U/LIRGs is a likely cause of a unique structure of buried AGNs, whose amount of material may be maintained through merger-induced supply from their host galaxies.

DOI： 10.3847/1538-4357/ad2936

Scopus

Naomichi Yutani, Yoshiki Toba, Keiichi Wada .  Apparent Effect of Dust Extinction on the Observed Outflow Velocity of Ionized Gas in Galaxy Mergers .  The Astrophysical Journal961 ( 1 ) 68 - 68   2024年1月査読

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担当区分：責任著者   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

In this study, we examine photoionization outflows during the late stages of galaxy mergers, with a specific focus on the relation between the observed velocity of outflowing gas and the apparent effects of dust extinction. We used the N-body/smoothed particle hydrodynamics code ASURA for galaxy merger simulations. These simulations concentrated on identical galaxy mergers featuring supermassive black holes of 10⁸ M _⊙ and gas fractions of 30% and 10%. From the simulation data, we derived velocity and velocity dispersion diagrams for the active galactic nuclei (AGN)-driven ionized outflowing gas. Our findings show that high-velocity outflows with velocity dispersions of 500 km s⁻¹ or greater can be observed in the late stages of galactic mergers. Particularly, in buried AGNs, both the luminosity-weighted outflow velocity and velocity dispersion increase owing to the apparent effects of dust extinction. Owing to these effects, velocity–velocity dispersion diagrams display a noticeable blue-shifted tilt in models with higher gas fractions. Crucially, this tilt is not influenced by the AGN luminosity but emerges from the observational impacts of dust extinction. Our results imply that the observed high-velocity [O iii] λ5007 outflow exceeding 1000 km s⁻¹ in buried AGNs may be linked to the dust extinction that occurs during the late stages of gas-rich galaxy mergers.

DOI： 10.3847/1538-4357/ad0dfc

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ad0dfc/pdf

Wada, Keiichi; Kudoh, Yuki ; Nagao, Tohru .  Multi-phase gas nature in the sub-pc region of the active galactic nuclei II: Possible origins of the changing-state AGNs" .  Monthly Notices of the Royal Astronomical Society526 ( 2 ) 2717 - 2723   2023年12月査読

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担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1093/mnras/stad2918

Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, and Shoji Ogawa .  Circumnuclear Multi-phase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy .  The Astrophysical Journal958   150   2023年11月査読

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記述言語：英語  

DOI： 10.3847/1538-4357/ad06ac

Takuma Izumi, Keiichi Wada, Masatoshi Imanishi, Kouichiro Nakanishi, Kotaro Kohno, Yuki Kudoh, Taiki Kawamuro, Shunsuke Baba, Naoki Matsumoto, Yutaka Fujita, Konrad R. W. Tristram .  Supermassive black hole feeding and feedback observed on subparsec scales .  Science382 ( 6670 ) 554 - 559   2023年11月査読

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掲載種別：研究論文（学術雑誌）   出版者・発行元：American Association for the Advancement of Science (AAAS)  

Active galaxies contain a supermassive black hole at their center that grows by accreting matter from the surrounding galaxy. The accretion process in about the central 10 parsecs has not been directly resolved in previous observations because of the small apparent angular sizes involved. We observed the active nucleus of the Circinus Galaxy using submillimeter interferometry. A dense inflow of molecular gas was evident on subparsec scales. We calculated that less than 3% of this inflow is accreted by the black hole, with the rest being ejected by multiphase outflows, providing feedback to the host galaxy. Our observations also reveal a dense gas disk surrounding the inflow that is gravitationally unstable, which drives the accretion into about the central 1 parsec.

DOI： 10.1126/science.adf0569

Kosei Matsumoto, Peter Camps, Maarten Baes, Frederik De Ceuster, Keiichi Wada, Takao Nakagawa, Kentaro Nagamine .  Self-consistent dust and non-LTE line radiative transfer with SKIRT .  Astronomy & Astrophysics   2023年10月査読

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掲載種別：研究論文（学術雑誌）  

DOI： 10.1051/0004-6361/202347376

Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura .  Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. I. Dynamical Structures of Dusty and Dust-free Outflow .  The Astrophysical Journal950 ( 1 ) 72 - 72   2023年6月査読

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記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

We investigated dusty and dust-free gas dynamics for a radiation-driven sub-parsec-scale outflow in an active galactic nucleus (AGN) associated with a supermassive black hole 10⁷M_⊙ and bolometric luminosity 10⁴⁴ erg s⁻¹ based on the two-dimensional radiation-hydrodynamic simulations. A radiation-driven “lotus-like” multi-shell outflow is launched from the inner part (r ≲ 0.04 pc) of the geometrically thin disk, and it repeatedly and steadily produces shocks as mass accretion continues through the disk to the center. The shape of the dust sublimation radius is not spherical and depends on the angle (θ) from the disk plane, reflecting the nonspherical radiation field and nonuniform dust-free gas. Moreover, we found that the sublimation radius of θ ∼ 20°–60° varies on a timescale of several years. The “inflow-induced outflow” contributes to the obscuration of the nucleus in the sub-parsec region. The column density of the dust-free gas is N_H ≳ 10²² cm⁻² for r ≲ 0.04 pc. Gases near the disk plane (θ ≲ 30°) can be the origin of the Compton-thick component, which was suggested by the recent X-ray observations of AGNs. The dusty outflow from the sub-parsec region can be also a source of material for the radiation-driven fountain for a larger scale.

DOI： 10.3847/1538-4357/accc2b

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/accc2b/pdf

Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada .  Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers .  The Astrophysical Journal936 ( 2 ) 118 - 118   2022年9月査読

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掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

Dust-obscured galaxies (DOGs), which are observationally characterized as faint in the optical and bright in the infrared, are the final stage of galaxy mergers and are essential objects in the evolution of galaxies and active galactic nuclei (AGNs). However, the relationship between the torus-scale gas dynamics around AGNs and the DOGs’ lifetime remains unclear. We obtained the evolution of the spectral energy distributions (SEDs) of a galaxy merger system with AGN feedback from postprocessed pseudo-observations based on an N-body/smoothed particle hydrodynamics (SPH) simulation. We focused on a late-stage merger of two identical galaxies with a supermassive black hole (SMBH) of 10⁸M_⊙. We found that the infrared luminosity of the system reaches ultra- and hyperluminous infrared galaxy classes (10¹² and 10¹³L_⊙, respectively). The DOG phase corresponds to a state in which the AGNs are buried in dense gas and dust, with the infrared luminosity exceeding 3.3 × 10¹²L_⊙. We also identified subcategories of DOGs, namely bump and power-law DOGs, from the SEDs and their evolution. The bump DOGs tend to evolve to power-law DOGs over several Myrs. We found that contribution from the hot dust around the nucleus in the infrared radiation is essential for identifying the system as a power-law DOG; the gas and dust are distributed nonspherically around the nucleus, therefore, the observed properties of DOGs depend on the viewing angle. In our model, the lifetime of merger-driven DOGs is less than 4 Myr, suggesting that the observed DOG phase is a brief aspect of galaxy mergers.

DOI： 10.3847/1538-4357/ac87a2

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac87a2/pdf

Kosei Matsumoto, Takao Nakagawa, Keiichi Wada, Shunsuke Baba, Shusuke Onishi, Taisei Uzuo, Naoki Isobe, Yuki Kudoh .  Probing Dynamics and Thermal Properties Inside Molecular Tori with CO Rovibrational Absorption Lines .  The Astrophysical Journal934 ( 1 ) 25 - 39   2022年7月査読

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掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

A recent hydrodynamic model, the radiation-driven fountain model (Wada et al. 2016), presented a dynamical picture that active galactic nuclei (AGNs) tori sustain their geometrical thickness by gas circulation around AGNs, and previous papers have confirmed that this picture is consistent with multiwavelength observations of nearby Seyfert galaxies. Recent near-infrared observations implied that CO rovibrational absorption lines (ΔJ = ± 1, v = 0 − 1, λ ∼ 4.7 μm) could probe the physical properties of the inside tori. However, the origin of the CO absorption lines has been under debate. In this paper, we investigate the origin of the absorption lines and conditions for detecting them by performing line radiative transfer calculations based on the radiation-driven fountain model. We find that CO rovibrational absorption lines are detected at inclination angles θ_obs = 50°–80°. At the inclination angle θ_obs = 77°, we observe multi-velocity components: inflow (v_LOS = 30 km s⁻¹), systemic (v_LOS = 0 km s⁻¹), and outflows (v_LOS = −75, − 95, and −105 km s⁻¹). The inflow and outflow components (v_LOS = 30 and −95 km s⁻¹) are collisionally excited at the excitation temperatures of 186 and 380 K up to J = 12 and 4, respectively. The inflow and outflow components originate from the accreting gas on the equatorial plane at 1.5 pc from the AGN center and the outflowing gas driven by AGN radiation pressure at 1.0 pc, respectively. These results suggest that CO rovibrational absorption lines can provide us with the velocities and kinetic temperatures of the inflow and outflow in the inner few parsec region of AGN tori, and the observations can probe the gas circulation inside the tori.

DOI： 10.3847/1538-4357/ac755f

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac755f/pdf

Yoshiki Toba, Teng Liu, Tanya Urrutia, Mara Salvato, Junyao Li, Yoshihiro Ueda, Marcella Brusa, Naomichi Yutani, Keiichi Wada, Atsushi J. Nishizawa, Johannes Buchner, Tohru Nagao, Andrea Merloni, Masayuki Akiyama, Riccardo Arcodia, Bau-Ching Hsieh, Kohei Ichikawa, Masatoshi Imanishi, Kaiki T. Inoue, Toshihiro Kawaguchi, Georg Lamer, Kirpal Nandra, John D. Silverman, Yuichi Terashima .  The eROSITA Final Equatorial-Depth Survey (eFEDS) A multiwavelength view of WISE mid-infrared galaxies/active galactic nuclei .  ASTRONOMY & ASTROPHYSICS661   2022年5月査読

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記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：EDP SCIENCES S A  

Aims. We investigate the physical properties - such as the stellar mass (M-*), star-formation rate, infrared (IR) luminosity (L-IR), X-ray luminosity (L-X), and hydrogen column density (N-H) - of mid-IR (MIR) galaxies and active galactic nuclei (AGN) at z < 4 in the 140 deg(2) field observed by eROSITA on SRG using the Performance-and-Verification-Phase program named the eROSITA Final Equatorial Depth Survey (eFEDS).Methods. By cross-matching the WISE 22 mu m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROSITA. We have compiled a multiwavelength dataset extending from X-ray to far-IR wavelengths. We have also performed (i) an X-ray spectral analysis, (ii) spectral-energy-distribution fitting using X-CIGALE, (iii) 2D image-decomposition analysis using Subaru Hyper Suprime-Cam images, and (iv) optical spectral fitting with QSFit to investigate the AGN and host-galaxy properties. For 7088 WISE 22 tim objects that are undetected by eROSITA, we have performed an X-ray stacking analysis to examine the typical physical properties of these X-ray faint and probably obscured objects.Results. We find that (i) 82% of the eFEDS-W4 sources are classified as X-ray AGN with log L-X > 42 erg s(-1); (ii) 67 and 24% of the objects have log (L-IR/L-circle dot) > 12 and 13, respectively; (iii) the relationship between L-X and the 6 mu m luminosity is consistent with that reported in previous works; and (iv) the relationship between the Eddington ratio and N-H for the eFEDS-W4 sample and a comparison with a model prediction from a galaxy-merger simulation indicates that approximately 5.0% of the eFEDS-W4 sources in our sample are likely to be in an AGN-feedback phase, in which strong radiation pressure from the AGN blows out the surrounding material from the nuclear region.Conclusions. Thanks to the wide area coverage of eFEDS, we have been able to constrain the ranges of the physical properties of the WISE 22 mu m-selected sample of AGNs at z < 4, providing a benchmark for forthcoming studies on a complete census of MIR galaxies selected from the full-depth eROSITA all-sky survey.

DOI： 10.1051/0004-6361/202141547

Web of Science

Shinsuke Takasao, Yuri Shuto, Keiichi Wada .  Spontaneous Formation of Outflows Powered by Rotating Magnetized Accretion Flows in a Galactic Center .  The Astrophysical Journal926 ( 1 ) 50 - 50   2022年2月査読

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掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

<title>Abstract</title>
We investigate how magnetically driven outflows are powered by a rotating, weakly magnetized accretion flow onto a supermassive black hole using axisymmetric magnetohydrodynamic simulations. Our proposed model focuses on the accretion dynamics on an intermediate scale between the Schwarzschild radius and the galactic scale, which is ∼1–100 pc. We demonstrate that a rotating disk formed on a parsec-scale acquires poloidal magnetic fields via accretion, and this produces an asymmetric bipolar outflow at some point. The formation of the outflow was found to follow the growth of strongly magnetized regions around disk surfaces (magnetic bubbles). The bipolar outflow grew continuously inside the expanding bubbles. We theoretically derived the growth condition of the magnetic bubbles for our model that corresponds to a necessary condition for outflow growth. We found that the north–south asymmetrical structure of the bipolar outflow originates from the complex motions excited by accreting flows around the outer edge of the disk. The bipolar outflow comprises multiple mini-outflows and downflows (failed outflows). The mini-outflows emanate from the magnetic concentrations (magnetic patches). The magnetic patches exhibit inward drifting motions, thereby making the outflows unsteady. We demonstrate that the inward drift can be modeled using a simple magnetic patch model that considers magnetic angular momentum extraction. This study could be helpful for understanding how asymmetric and nonsteady outflows with complex substructures are produced around supermassive black holes without the help of strong radiation from accretion disks or entrainment by radio jets such as molecular outflows in radio-quiet active galactic nuclei, e.g., NGC 1377.

DOI： 10.3847/1538-4357/ac38a8

arXiv

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac38a8/pdf

Ogawa, Shoji; Ueda, Yoshihiro; Wada, Keiichi; Mizumoto, Misaki .  Warm Absorbers in the Radiation-driven Fountain Model of Low-mass Active Galactic Nuclei .  The Astrophysical Journal925 ( 1 ) 55   2022年1月査読

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記述言語：英語  

DOI： 10.3847/1538-4357/ac3cb9

Toba, Yoshiki ; Liu, Teng search by orcid ; Urrutia, Tanya ; Salvato, Mara ; Li, Junyao ; Ueda, Yoshihiro ; Brusa, Marcella ; Yutani, Naomichi ; Wada, Keiichi ; Nishizawa, Atsushi J. ; Buchner, Johannes search by orcid ; Nagao, Tohru ; Merloni, Andrea ; Akiyama, Masayuki ; Arcodia, Riccardo ; Hsieh, Bau-Ching ; Ichikawa, Kohei ; Imanishi, Masatoshi ; Inoue, Kaiki T. ; Kawaguchi, Toshihiro ; Lamer, Georg ; Nandra, Kirpal ; Silverman, John D. ; Terashima, Yuichi .  The eROSITA Final Equatorial-Depth Survey (eFEDS): A multiwavelength view of WISE mid-infrared galaxies/active galactic nuclei .  Astronomy and Astrophysics649   2021年8月国際共著

Kazuma Joh, Tohru Nagao, Keiichi Wada, Koki Terao, Takuji Yamashita .  Do gas clouds in narrow-line regions of Seyfert galaxies come from their nuclei? .  Publications of the Astronomical Society of Japan73 ( 4 ) 1152 - 1165   2021年8月査読

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1093/pasj/psab065

García-Burillo, S. ; Alonso-Herrero, A. ; Ramos Almeida, C. search by orcid ; González-Martín, O. ; Combes, F. ; Usero, A. search by orcid ; Hönig, S. ; Querejeta, M. ; Hicks, E. K. S. ; Hunt, L. K. search by orcid ; Rosario, D. ; Davies, R. search by orcid ; Boorman, P. G. search by orcid ; Bunker, A. J. ; Burtscher, L. ; Colina, L. ; Díaz-Santos, T. search by orcid ; Gandhi, P. ; García-Bernete, I. ; García-Lorenzo, B. ; Ichikawa, K. ; Imanishi, M. ; Izumi, T. ; Labiano, A. ; Levenson, N. A. ; López-Rodríguez, E. ; Packham, C. search by orcid ; Pereira-Santaella, M. ; Ricci, C. ; Rigopoulou, D. ; Rouan, D. ; Shimizu, T. ; Stalevski, M. ; Wada, K. ; Williamson, D. Abstract .  The Galaxy Activity, Torus, and Outflow Survey (GATOS). I. ALMA images of dusty molecular tori in Seyfert galaxies .  Astronomy & Astrophysics652   A98   2021年8月国際共著

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DOI： 10.1051/0004-6361/202141075

Alonso-Herrero, A. ; García-Burillo, S. ; Hönig, S. F. ; García-Bernete, I. ; Ramos Almeida, C. search by orcid ; González-Martín, O. ; López-Rodríguez, E. ; Boorman, P. G. search by orcid ; Bunker, A. J. ; Burtscher, L. ; Combes, F. ; Davies, R. search by orcid ; Díaz-Santos, T. search by orcid ; Gandhi, P. ; García-Lorenzo, B. ; Hicks, E. K. S. ; Hunt, L. K. search by orcid ; Ichikawa, K. ; Imanishi, M. ; Izumi, T. ; Labiano, A. ; Levenson, N. A. ; Packham, C. search by orcid ; Pereira-Santaella, M. ; Ricci, C. ; Rigopoulou, D. ; Roche, P. search by orcid ; Rosario, D. J. ; Rouan, D. ; Shimizu, T. search by orcid ; Stalevski, M. search by orcid ; Wada, K. ; Williamson, D. .  The Galaxy Activity, Torus, and Outflow Survey (GATOS). II. Torus and polar dust emission in nearby Seyfert galaxies .  Astronomy & Astrophysics652   A99   2021年8月査読 国際共著

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

We compare high angular resolution mid-infrared (mid-IR) and Atacama Large Millimeter/submillimeter Array (ALMA) far-infrared (far-IR) images of twelve nearby (median 21 Mpc) Seyfert galaxies selected from the Galaxy Activity, Torus, and Outflow Survey (GATOS). The mid-IR unresolved emission contributes more than 60% of the nuclear (diameters of 1.5″ ∼ 150 pc) emission in most galaxies. By contrast, the ALMA 870  μm continuum emission is mostlyresolved with a median diameter of 42 pc and typically along the equatorial direction of the torus (Paper I). The Eddington ratios and nuclear hydrogen column densities (NH) of half the sample are favorable to launching polar and/or equatorial dusty winds, according to numerical simulations. Six of these show mid-IR extended emission approximately in the polar direction as traced by the narrow line region and perpendicular to the ALMA emission. In a few galaxies, the nuclear NH might be too high to uplift large quantities of dusty material along the polar direction. Five galaxies have low NH and/or Eddington ratios and thus polar dusty winds are not likely. We generated new radiative transfer CAT3D-WIND disk+wind models and model images at 8, 12, and 700  μm. We tailored these models to the properties of the GATOS Seyferts in this work. At low wind-to-disk cloud ratios, the far-IR model images have disk-and ring-like morphologies. The characteristic "X"-shape associated with dusty winds is seen better in the far-IR at intermediate-high inclinations for the extended-wind configurations. In most of the explored models, the mid-IR emission mainly comes from the inner part of the disk and cone. Extended biconical and one-sided polar mid-IR emission is seen in extended-wind configurations and high wind-to-disk cloud ratios. When convolved to the typical angular resolution of our observations, the CAT3D-WIND model images reproduce qualitative aspects of the observed mid-and far-IR morphologies. However, low to intermediate values of the wind-to-disk ratio are required to account for the observed large fractions of unresolved mid-IR emission in our sample. This work and Paper I provide observational support for the torus+wind scenario. The wind component is more relevant at high Eddington ratios and/or active galactic nucleus luminosities, and polar dust emission is predicted at nuclear column densities of up to ∼1024 cm-2. The torus or disk component, on the other hand, prevails at low luminosities and/or Eddington ratios.

DOI： 10.1051/0004-6361/202141219

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