XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

Tanimoto, A.; Ueda, Yoshihiro; Odaka, Hirokazu; Kawaguchi, Toshihiro; Fukazawa, Yasushi; Kawamuro, T.

doi:10.3847/1538-4357/ab1b20

Cited by 84 publications

(108 citation statements)

References 105 publications

(127 reference statements)

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“…For the torus or disk component, we list in Table 3 the estimated inclinations using fits to the high angular resolution IR SEDs and mid-IR spectroscopy using the clumpy models (Nenkova et al 2008a,b) and fits to the Spitzer/IRS spectroscopy with the CAT3D-WIND torus models (Hönig & Kishimoto 2017). We also included the inclination values derived from fits to the X-ray emission using the xclumpy model (Tanimoto et al 2019(Tanimoto et al , 2020Ogawa et al 2021). Additionally, there are lower limits to the torus inclination based on the ellipticity of the ALMA extended 870 µm continuum images from GB21.…”

Section: Summary Of Torus and Wind Properties Of The Samplementioning

confidence: 99%

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: Summary Of Torus and Wind Properties Of The Samplementioning

confidence: 99%

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

Alonso‐Herrero

García‐Burillo

Hönig

et al. 2021

A&A

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“…Despite its popularity in the literature, the pexrav model we employed here does not have the correct geometry to properly represent the torus. Spectral models for reprocessing in the torus exhibit a greater range in the shape and amplitude of the Compton hump (e.g., Paltani & Ricci 2017;Buchner et al 2019;Tanimoto et al 2019). In future publications we will use modern spectral models from the BORUS suite (Baloković et al 2018(Baloković et al , 2019 that self-consistently account for the cutoff in the coronal continuum, as well as the reprocessing features from the torus.…”

Section: Limitations and Future Workmentioning

confidence: 99%

NuSTAR Survey of Obscured Swift/BAT-selected Active Galactic Nuclei. II. Median High-energy Cutoff in Seyfert II Hard X-Ray Spectra

Baloković

Harrison

Madejski

et al. 2020

ApJ

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Broadband X-ray spectroscopy of the X-ray emission produced in the coronae of active galactic nuclei (AGNs) can provide important insights into the physical conditions very close to their central supermassive black holes. The temperature of the Comptonizing plasma that forms the corona is manifested through a high-energy cutoff that has been difficult to directly constrain even in the brightest AGN because it requires high-quality data at energies above 10 keV. In this paper we present a large collection of coronal cutoff constraints for obscured AGNs based on a sample of 130AGNs selected in the hard X-ray band with Swift/BAT and observed nearly simultaneously with NuSTAR and Swift/XRT. We find that under a reasonable set of assumptions regarding partial constraints the median cutoff is well constrained to 290±20 keV, where the uncertainty is statistical and given at the 68% confidence level. We investigate the sensitivity of this result to our assumptions and find that consideration of various known systematic uncertainties robustly places the median cutoff between 240 and 340 keV. The central 68% of the intrinsic cutoff distribution is found to be between about 140 and 500 keV, with estimated uncertainties of 20 and 100 keV, respectively. In comparison with the literature, we find no clear evidence that the cutoffs in obscured and unobscured AGNs are substantially different. Our analysis highlights the importance of carefully considering partial and potentially degenerate constraints on the coronal high-energy cutoff in AGNs.Unified Astronomy Thesaurus concepts: Active galactic nuclei (16); X-ray active galactic nuclei (2035); Seyfert galaxies (1447); High energy astrophysics (739); X-ray surveys (1824)

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“…The winds provide additional obscuration traced by covering factors and could separate the obscured and unobscured regions, and thus separate Type-1 and Type-2 AGNs. Similarly, Ogawa et al ( 2021 ) describe a disc wind model analogous to H önig ( 2019 ) using X-CLUMPY (Nenkova et al 2008 ;Tanimoto et al 2019 ), another SED toroidal model. In that work, X-CLUMPY is used in two different models for obscured and unobscured A GNs.…”

Section: The Agn Dust Windsmentioning

confidence: 99%

“…Mullaney et al 2011 ;Bernhard et al 2021 ) or AGN models (e.g. Pier & Krolik 1992 ;Granato & Danese 1994 ;Efstathiou & Rowan-Robinson 1995 ;Fritz, Franceschini & Hatziminaoglou 2006 ;Nenkova et al 2008 ;Stalevski et al 2012Stalevski et al , 2016Siebenmorgen, Heymann & Efstathiou 2015 ;Tanimoto et al 2019 ), which are fitted together with dust emissions and stellar populations (e.g. Calistro Rivera et al 2016 ;Leja et al 2018 ;Boquien et al 2019 ) in different configurations (check Thorne et al 2021 ;P érez-Torres et al 2021 , for an o v erview of the most popular SED fitting codes).…”

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confidence: 99%

The viewing angle in AGN SED models: a data-driven analysis

Padilla

Wang

Małek

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The validity of the unified active galactic nuclei (AGN) model has been challenged in the last decade, especially when different types of AGNs are considered to only differ in the viewing angle to the torus. We aim to assess the importance of the viewing angle in classifying different types of Seyfert galaxies in spectral energy distribution (SED) modelling. We retrieve photometric data from publicly available astronomical databases: CDS and NED, to model SEDs with X-CIGALE in a sample of 13 173 Seyfert galaxies located at redshift range from z = 0 to z = 3.5, with a median redshift of z ≈ 0.2. We assess whether the estimated viewing angle from the SED models reflects different Seyfert classifications. Two AGN models with either a smooth or clumpy torus structure are adopted in this paper. We find that the viewing angle in Type-1 AGNs is better constrained than in Type-2 AGNs. Limiting the viewing angles representing these two types of AGNs do not affect the physical parameter estimates such as star-formation rate (SFR) or AGN fractional contribution (fAGN). In addition, the viewing angle is not the most discriminating physical parameter to differentiate Seyfert types. We suggest that the observed and intrinsic AGN disc luminosity can: i) be used in z < 0.5 studies to distinguish between Type-1 and Type-2 AGNs, and ii) explain the probable evolutionary path between these AGN types. Finally, we propose the use of X-CIGALE for AGN galaxy classification tasks. All data from the 13 173 SED fits are available at Zenodo.†

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XCLUMPY: X-Ray Spectral Model from Clumpy Torus and Its Application to the Circinus Galaxy

Cited by 84 publications

References 105 publications

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

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

NuSTAR Survey of Obscured Swift/BAT-selected Active Galactic Nuclei. II. Median High-energy Cutoff in Seyfert II Hard X-Ray Spectra

The viewing angle in AGN SED models: a data-driven analysis

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