GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei

Abstract The polar mid-infrared (MIR) emission detected within tens to hundreds of parsecs in some active galactic nuclei (AGN) has been associated with dusty winds driven away by radiation pressure. The physical characterization of this extended polar emission remains uncertain. Here, we combine 10–21 μ m JWST/Mid-InfRared Instrument (MIRI) imaging observations with 7–25 μ m JWST/MIRI MRS integral field spectroscopic observations of six nearby, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>D</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>¯</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:mn>35.4</mml:mn> <mml:mo>±</mml:mo> <mml:mn>4.6</mml:mn> </mml:math> Mpc, AGN from the GATOS Survey to quantify the nature of the extended MIR emission at ∼75 pc resolution at 21 μ m. These AGN have similar bolometric luminosities, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>log</mml:mi> <mml:mn>10</mml:mn> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mover accent="true"> <mml:mi>L</mml:mi> <mml:mo>¯</mml:mo> </mml:mover> <mml:mi>bol</mml:mi> </mml:msub> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">[</mml:mo> <mml:msup> <mml:mrow> <mml:mi>erg</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathvariant="normal">s</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">]</mml:mo> <mml:mo stretchy="false">)</mml:mo> <mml:mspace width="0.25em"/> <mml:mo>=</mml:mo> <mml:mspace width="0.25em"/> <mml:mn>44.0</mml:mn> <mml:mspace width="0.25em"/> <mml:mo>±</mml:mo> <mml:mspace width="0.25em"/> <mml:mn>0.3</mml:mn> </mml:math> , span a wide range of optical outflow rates, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> </mml:math> 0.003–0.21 M ⊙ yr −1 , column densities, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>log</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">X</mml:mi> <mml:mo>−</mml:mo> <mml:mi mathvariant="normal">ray</mml:mi> </mml:mrow> </mml:msubsup> <mml:mo stretchy="false">[</mml:mo> <mml:msup> <mml:mrow> <mml:mi mathvariant="normal">cm</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">]</mml:mo> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> </mml:math> 22.2–24.3, and Eddington ratios, λ Edd = 0.005–0.06. We cross-correlate the line-only and continuum-only images and find a poor correlation, which indicates that the extended MIR continuum emission is spatially uncorrelated with the warm outflows associated with narrow emission lines within 10–15 μ m. Line emission is resolved along the jet axis, while dust emission is perpendicular to it. The 75–450 pc continuum emission has a fairly constant dust temperature, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">d</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>13</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>7</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>7</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> K, and mass, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">d</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>72</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>27</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>29</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> M ⊙ . Using the conditions of energy balance between

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The Astrophysical Journal
Published
2025-11-26
DOI
https://doi.org/10.3847/1538-4357/ae0187
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1
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Astrophysics and Star Formation Studies
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article

GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei

Takuma Izumi, Lindsay Fuller, S. Hoenig, D. J. Rosario et al.
1 citations
The Astrophysical Journal
Astrophysics and Star Formation Studies
1.15
article

GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei

Takuma Izumi, Lindsay Fuller, S. Hoenig, D. J. Rosario, C. Packham, I. García-Bernete, Cláudio Ricci, Robert Nikutta, A. Alonso‐Herrero, C. Ramos Almeida, Alvaro Labiano, N. A. Levenson, E. K. S. Hicks, A. Audibert, S. García‐Burillo, R. Davies, B. García‐Lorenzo, M. J. Ward, Donají Esparza-Arredondo, Lulu Zhang, Steph Campbell, Masatoshi Imanishi, Thomas Shimizu, D. Rigopoulou, Kohei Ichikawa, F. Combes, Enrique López-Rodríguez, M. Pereira-Santaella, Andrew J. Bunker, Daniel Rouan, P. Gandhi, Marko Stalevski, E. Bellocchi, O. González-Martín, T. Díaz-Santos
article en
1 citations

Abstract

Abstract The polar mid-infrared (MIR) emission detected within tens to hundreds of parsecs in some active galactic nuclei (AGN) has been associated with dusty winds driven away by radiation pressure. The physical characterization of this extended polar emission remains uncertain. Here, we combine 10–21 μ m JWST/Mid-InfRared Instrument (MIRI) imaging observations with 7–25 μ m JWST/MIRI MRS integral field spectroscopic observations of six nearby, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>D</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>¯</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> <mml:mn>35.4</mml:mn> <mml:mo>±</mml:mo> <mml:mn>4.6</mml:mn> </mml:math> Mpc, AGN from the GATOS Survey to quantify the nature of the extended MIR emission at ∼75 pc resolution at 21 μ m. These AGN have similar bolometric luminosities, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>log</mml:mi> <mml:mn>10</mml:mn> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mover accent="true"> <mml:mi>L</mml:mi> <mml:mo>¯</mml:mo> </mml:mover> <mml:mi>bol</mml:mi> </mml:msub> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">[</mml:mo> <mml:msup> <mml:mrow> <mml:mi>erg</mml:mi> <mml:mspace width="0.25em"/> <mml:mi mathvariant="normal">s</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">]</mml:mo> <mml:mo stretchy="false">)</mml:mo> <mml:mspace width="0.25em"/> <mml:mo>=</mml:mo> <mml:mspace width="0.25em"/> <mml:mn>44.0</mml:mn> <mml:mspace width="0.25em"/> <mml:mo>±</mml:mo> <mml:mspace width="0.25em"/> <mml:mn>0.3</mml:mn> </mml:math> , span a wide range of optical outflow rates, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mover accent="true"> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>̇</mml:mo> </mml:mrow> </mml:mover> <mml:mo>=</mml:mo> </mml:math> 0.003–0.21 M ⊙ yr −1 , column densities, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>log</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy="false">(</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">X</mml:mi> <mml:mo>−</mml:mo> <mml:mi mathvariant="normal">ray</mml:mi> </mml:mrow> </mml:msubsup> <mml:mo stretchy="false">[</mml:mo> <mml:msup> <mml:mrow> <mml:mi mathvariant="normal">cm</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> <mml:mo stretchy="false">]</mml:mo> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> </mml:math> 22.2–24.3, and Eddington ratios, λ Edd = 0.005–0.06. We cross-correlate the line-only and continuum-only images and find a poor correlation, which indicates that the extended MIR continuum emission is spatially uncorrelated with the warm outflows associated with narrow emission lines within 10–15 μ m. Line emission is resolved along the jet axis, while dust emission is perpendicular to it. The 75–450 pc continuum emission has a fairly constant dust temperature, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">d</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>13</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>7</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>7</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> K, and mass, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">d</mml:mi> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>72</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>27</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>29</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> M ⊙ . Using the conditions of energy balance between

The Astrophysical JournalVol. 994(2)
University of Geneva (CH), Universidad Complutense de Madrid (ES), Centre National de la Recherche Scientifique (FR), Space Telescope Science Institute (US), University of Alaska Fairbanks (US), University of Alaska Anchorage (US), Waseda University (JP), University of South Carolina (US), Universidad de La Laguna (ES), Durham University (GB), National Institutes of Natural Sciences (JP), The Graduate University for Advanced Studies, SOKENDAI (JP), European University Cyprus (CY), Peking University (CN), Université Paris Sciences et Lettres (FR), Observatoire de Paris (FR), European Space Agency (FR), Ghent University (BE), Sorbonne Université (FR), University of Oxford (GB), Sorbonne Paris Cité (FR), Max Planck Institute for Extraterrestrial Physics (DE), European Space Astronomy Centre (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Instituto de Física Fundamental (ES), Kavli Institute for Theoretical Sciences (CN), Université Bourgogne Franche-Comté (FR), Laboratoire d’études spatiales et d’instrumentation en astrophysique (FR), Centro de Astrobiología (ES), Instituto de Astrofísica de Canarias (ES), Community Science and Data Center (US), NSF NOIRLab (US), Spanish National Observatory (ES), Astronomical Observatory (RS), National Astronomical Observatory of Japan (JP), University of Southampton (GB), The University of Texas at San Antonio (US), Newcastle University (GB), Foundation for Research and Technology Hellas (GR), Universidad Nacional Autónoma de México (MX), Universidad Diego Portales (CL), Stanford University (US)
National Aeronautics and Space Administration, Comunidad de Madrid, Space Telescope Science Institute, European Commission, Nuclear Safety and Security Commission, Ministerio de Ciencia e Innovación, European Regional Development Fund, Agencia Estatal de Investigación, Astrophysics Division
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Astrophysics and Star Formation Studies
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