Torus model properties of an ultra-hard X-ray selected sample of Seyfert galaxies

García-Bernete, I.; Almeida, C. Ramos; Alonso‐Herrero, A.; Ward, M. J.; Acosta–Pulido, J. A.; Pereira-Santaella, M.; Hernán-Caballero, A.; Ramos, A. Asensio; González‐Martín, O.; Levenson, N. A.; Mateos, S.; Carrera, Francisco J.; Ricci, Cláudio; Roche, P. F.; Márquez, I.; Packham, C.; Masegosa, J.; Fuller, Lindsay

doi:10.1093/mnras/stz1003

Cited by 44 publications

(51 citation statements)

References 143 publications

(153 reference statements)

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“…Torus models also incorporated an additional polar dust component to account for the mid-IR imaging and interferometric observations of some Seyfert galaxies Gallagher et al 2015;Hönig & Kishimoto 2017;Stalevski et al 2017;Isbell et al 2021). These models reproduced satisfactorily the observed nuclear IR emission of samples of nearby AGN (see e.g., Ramos Almeida et al 2009Alonso-Herrero et al 2011;Ichikawa et al 2015;García-González et al 2017;García-Bernete et al 2019;González-Martín et al 2019). Elitzur & Shlosman (2006) put forward a scenario where the torus is part of a clumpy outflow, and recently Venanzi et al (2020) demonstrated theoretically that dusty winds can be launched at the inner walls of the torus.…”

Section: Introductionmentioning

confidence: 86%

The Galaxy Activity, Torus, and Outflow Survey (GATOS)

Alonso‐Herrero

García‐Burillo

Hönig

et al. 2021

A&A

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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.

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Section: Introductionmentioning

confidence: 86%

The Galaxy Activity, Torus, and Outflow Survey (GATOS)

Alonso‐Herrero

García‐Burillo

Hönig

et al. 2021

A&A

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“…However, as shown in this paper, when this contribution is large (stellar component contributing at least 50% compared to the torus component at 5 µm, or dust heated by star-formation contributing at least 50% compared to the torus component at 30 µm) dilution strongly influences the parameter determination. High spatial resolution observations are needed for the best isolation of the dust associated the AGN from other contributors, as those provided with ground-based facilities (Ramos Almeida et al 2009;Fuller et al 2016;Martínez-Paredes et al 2017;García-Bernete et al 2019), the novel combination of VLTI+GRAVITY and the future JWST. Note however that both N-and Q-bands groundbased spectra are available only for NGC 1068.…”

Section: Goodness Of Parameter Determinationmentioning

confidence: 99%

Exploring the Mid-infrared SEDs of Six AGN Dusty Torus Models. II. The Data

González‐Martín¹,

Masegosa

García-Bernete

et al. 2019

ApJ

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This is the second in a series of papers devoted to explore a set of six dusty models of active galactic nuclei (AGN) with available spectral energy distributions (SEDs). These models are the smooth torus by Fritz et al. (2006), the clumpy torus by Nenkova et al. (2008B), the clumpy torus by , the two phase torus by Siebenmorgen et al. (2015), the two phase torus by Stalevski et al. (2016), and the wind model by Hönig & Kishimoto (2017). The first paper explores discrimination among models and the parameter restriction using synthetic spectra (González-Martín et al. 2019A). Here we perform spectral fitting of a sample of 110 AGN drawn from the Swift/BAT survey with Spitzer /IRS spectroscopic data. The aim is to explore which is the model that describes better the data and the resulting parameters. The clumpy wind-disk model by Hönig & Kishimoto (2017) provides good fits for ∼50% of the sample, and the clumpy torus model by Nenkova et al. (2008B) is good at describing ∼30% of the objects. The wind-disk model by Hönig & Kishimoto (2017) is better for reproducing the mid-infrared spectra of Type-1 Seyferts (with 60% of the Type-1 Seyferts well reproduced by this model compared to the 10% well represented by the clumpy torus model by Nenkova et al. 2008B) while Type-2 Seyferts are equally fitted by both models (roughly 40% of the Type-2 Seyferts). Large residuals are found irrespective of the model used, indicating that the AGN dust continuum emission is more complex than predicted by the models or that the parameter space is not well sampled. We found that all the resulting parameters for our AGN sample are roughly constrained to 10-20% of the parameter space. Contrary to what is generally assumed, the derived outer radius of the torus is smaller (reaching up to a factor of ∼ 5 times smaller for 10 pc tori) for the smooth torus by Fritz et al. (2006) and the two phase torus by Stalevski et al. (2016) than the one derived from the clumpy torus by (Nenkova et al. 2008B). Covering factors and line-of-sight viewing angles strongly depend on the model used. The total dust mass is the most robust derived quantity, giving equivalent results for four of these models.

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“…A large body of work using SED fits to local AGNs (e.g., Ramos Almeida et al 2009;Alonso-Herrero et al 2011;Lira et al 2013;García-González et al 2016;García-Bernete et al 2019;Martínez-Paredes et al 2020) suggests that L and M observations at high sensitivity and angular resolution are required to study the physical properties of the 3-5 μm radiation bump. In fact, Lira et al (2013) emphasized that spectral information at 5 μm is necessary to properly constrain their SED fits.…”

Section: Introductionmentioning

confidence: 99%

Subarcsecond Mid-infrared View of Local Active Galactic Nuclei. IV. The L- and M-band Imaging Atlas*

Isbell

Burtscher²,

Asmus

et al. 2021

ApJ

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We present the largest currently existing subarcsecond 3–5 μm atlas of 119 local (z < 0.3) active galactic nuclei (AGNs). This atlas includes AGNs of five subtypes: 22 are Seyfert 1; five are intermediate Seyferts; 46 are Seyfert 2; 26 are low-ionization nuclear emission regions; and 20 are composites/starbursts. Each active galactic nucleus was observed with the Very Large Telescope Infrared Spectrometer and Array Camera (ISAAC) in the L and/or M bands between 2000 and 2013. We detected at 3σ confidence 92 sources in the L band and 83 sources in the M band. We separated the flux into unresolved nuclear flux and resolved the flux through two-Gaussian fitting. We report the nuclear flux, extended flux, apparent size, and position angle of each source, giving 3σ upper limits for sources that are undetected. Using Wide-field Infrared Survey Explorer (WISE) W1- and W2-band photometry we derived relations predicting the nuclear L and M fluxes for Sy1 and Sy2 AGNs based on their W1–W2 color and WISE fluxes. Lastly, we compare the measured mid-infrared colors to those predicted by dusty torus models SKIRTOR, CLUMPY, CAT3D, and CAT3D-WIND, finding the best agreement with the latter. We find that models including polar winds best reproduce the 3–5 μm colors, indicating that it is an important component of dusty torus models. We found that several AGNs are bluer than models predict. We discuss several explanations for this and find that it is most plausibly stellar light contamination within the ISAAC L-band nuclear fluxes.

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Torus model properties of an ultra-hard X-ray selected sample of Seyfert galaxies

Cited by 44 publications

References 143 publications

The Galaxy Activity, Torus, and Outflow Survey (GATOS)

The Galaxy Activity, Torus, and Outflow Survey (GATOS)

Exploring the Mid-infrared SEDs of Six AGN Dusty Torus Models. II. The Data

Subarcsecond Mid-infrared View of Local Active Galactic Nuclei. IV. The L- and M-band Imaging Atlas*

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