ISOTROPIC MID-INFRARED EMISSION FROM THE CENTRAL 100 pc OF ACTIVE GALAXIES

Levenson, N. A.; Radomski, J. T.; Packham, C.; Mason, Rachel; Schaefer, J. J.; Telesco, C. M.

doi:10.1088/0004-637x/703/1/390

Cited by 81 publications

(108 citation statements)

References 62 publications

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“…This method has been widely tested in ground-based MIR images (e.g. Soifer et al 2000;Radomski et al 2002Radomski et al , 2003Levenson et al 2009;Ramos Almeida et al 2009, 2011aMason et al 2012;García-Bernete et al 2015;Martínez-Paredes et al 2015). The MIR nuclear fluxes calculated using this method are listed in Table 2.…”

Section: Subarcsecond Resolution Nuclear Fluxes: Subtraction Of Scalementioning

confidence: 99%

“…On the other hand, due to the high energies involved in the accretion process, X-rays are good tracers of the AGN power. For this reason, the Xray MIR correlation has been widely used in the literature to investigate the origin of the MIR emission in different types of AGN (Lutz et al 2004;Ramos Almeida et al 2007;Horst et al 2008;Gandhi et al 2009;Levenson et al 2009;Ichikawa et al 2012;Mason et al 2012;Matsuta et al 2012;Sazonov et al 2012;Asmus et al 2015;Mateos et al 2015).…”

Section: Mir Correlations With Agn and Sf Indicatorsmentioning

confidence: 99%

“…Lutz et al 2004;Ramos Almeida et al 2007;Horst et al 2008;Gandhi et al 2009;Levenson et al 2009;Sazonov et al 2012). For example, Ramos Almeida et al (2007) found a slope of 0.8 by using nuclear fluxes obtained from ISOCAM data at 6.75 µm.…”

Section: Mir Correlations With Agn and Sf Indicatorsmentioning

confidence: 99%

“…Tristram et al 2009;Burtscher et al 2013), this angular resolution is fundamental to isolate its emission from other emitting sources at larger scales, as well as to disentangle the heating source of the diffuse circumnuclear MIR emission. However, our understanding about the dominant heating source of the dust on these physical scales (inner kpcs) remains unclear, because of the paucity of ground-based MIR instruments and the limited size of the samples studied to date (Horst et al 2008;Gandhi et al 2009;Levenson et al 2009;Mason et al 2012;González-Martín et al 2013). A major step forward was attained with the publication of the subarcsecond MIR imaging atlas of local AGN (Asmus et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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The nuclear and extended mid-infrared emission of Seyfert galaxies

García-Bernete¹,

Almeida²,

Acosta–Pulido³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present subarcsecond resolution mid-infrared (MIR) images obtained with 8-10 m-class ground-based telescopes of a complete volume-limited (D L <40 Mpc) sample of 24 Seyfert galaxies selected from the Swift/BAT nine month catalog. We use those MIR images to study the nuclear and circumnuclear emission of the galaxies. Using different methods to classify the MIR morphologies on scales of ∼400 pc, we find that the majority of the galaxies (75-83%) are extended or possibly extended and 17-25% are point-like. This extended emission is compact and it has low surface brightness compared with the nuclear emission, and it represents, on average, ∼30% of the total MIR emission of the galaxies in the sample. We find that the galaxies whose circumnuclear MIR emission is dominated by star formation show more extended emission (650±700 pc) than AGN-dominated systems (300±100 pc). In general, the galaxies with point-like MIR morphologies are face-on or moderately inclined (b/a∼0.4-1.0), and we do not find significant differences between the morphologies of Sy1 and Sy2. We used the nuclear and circumnuclear fluxes to investigate their correlation with different AGN and SF activity indicators. We find that the nuclear MIR emission (the inner ∼70 pc) is strongly correlated with the X-ray emission (the harder the X-rays the better the correlation) and with the [O IV] λ25.89 µm emission line, indicating that it is AGN-dominated. We find the same results, although with more scatter, for the circumnuclear emission, which indicates that the AGN dominates the MIR emission in the inner ∼400 pc of the galaxies, with some contribution from star formation.

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Section: Subarcsecond Resolution Nuclear Fluxes: Subtraction Of Scalementioning

confidence: 99%

Section: Mir Correlations With Agn and Sf Indicatorsmentioning

confidence: 99%

Section: Mir Correlations With Agn and Sf Indicatorsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The nuclear and extended mid-infrared emission of Seyfert galaxies

García-Bernete¹,

Almeida²,

Acosta–Pulido³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

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“…small dispersion between type 1 and type 2 AGN in the L MIR − L X -correlation) can be explained within the framework of a clumpy torus (e.g. Hönig et al 2006;Horst et al 2008;Nenkova et al 2008;Gandhi et al 2009;Levenson et al 2009). There is an interesting point to consider though: While IC 5063, ESO 323-G77, and MCG-3-34-64 are outliers in the L MIR − L X -correlation (see Fig.…”

Section: Mid-ir Continuum Emission and Its Relation To Agn Luminositymentioning

confidence: 99%

The dusty heart of nearby active galaxies

Hoenig

Kishimoto

Gandhi

et al. 2010

A&A

154

135

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In a series of papers, we aim at stepping towards characterizing physical properties of the AGN dust torus by combining IR highspatial resolution observations with 3D clumpy torus models. In this first paper, we present mid-IR imaging and 8−13 μm lowresolution spectroscopy of nine type 1 and ten type 2 AGN. The observations were carried out with the VLT/VISIR mid-IR imager and spectrograph and can be considered the largest currently available mid-infrared spectro-photometric data set of AGN at spatial resolution < ∼ 100 pc. These data resolve scales at which the emission from the dust torus dominates the overall flux, and emission from the host galaxy (e.g. star-formation) is resolved out in most cases. The silicate absorption features are moderately deep and emission features, if seen at all, are shallow. The strongest silicate emission feature in our sample shows some notable shift of the central wavelength from the expected 9.7 μm (based on ISM extinction curves) to ∼10.5 μm. We compare the observed mid-IR luminosities of our objects to AGN luminosity tracers (X-ray, optical and [O iii] luminosities) and find that the mid-IR radiation is emitted quite isotropically. In two cases, IC 5063 and MCG-3-34-64, we find evidence for extended dust emission in the narrow-line region. We confirm the correlation between observed silicate feature strength and Hydrogen column density, which was recently found in Spitzer data at lower spatial resolution. In a further step, our 3D clumpy torus model has been used to interpret the data. We show that the strength of the silicate feature and the mid-IR spectral index α can be used to get reasonable constraints on the radial dust distribution of the torus and the average number of clouds N 0 along an equatorial line-of-sight in clumpy torus models. The mid-IR spectral index α is almost exclusively determined by the radial dust distribution power-law index a, while the silicate feature depth mostly depends on N 0 and the torus inclination. A comparison of model predictions to our type 1 and type 2 AGN reveals that average parameters of a = −1.0 ± 0.5 and N 0 = 5 − 8 are typically seen in the presented sample, which means that the radial dust distribution is rather shallow. As a proof-of-concept of this method, we compared the model parameters derived from α and the silicate feature strength to more detailed studies of full IR SEDs and interferometry and found that the constraints on a and N 0 are consistent. Finally, we may have found evidence that the radial structure of the torus changes from low to high AGN luminosities towards steeper dust distributions, and we discuss implications for the IR size-luminosity relation.

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Introduction

Boorman

2020

The Accretion and Obscured Growth of Supermassive Black Holes

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ISOTROPIC MID-INFRARED EMISSION FROM THE CENTRAL 100 pc OF ACTIVE GALAXIES

Cited by 81 publications

References 62 publications

The nuclear and extended mid-infrared emission of Seyfert galaxies

The nuclear and extended mid-infrared emission of Seyfert galaxies

The dusty heart of nearby active galaxies

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