GATOS. VIII. On the physical origin of the extended MIR emission in AGN
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2025
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| author | Lopez-Rodriguez, Enrique Almeida, Cristina Ramos Pereira-Santaella, Miguel García-Bernete, Ismael Nikutta, Robert Alonso-Herrero, Almudena Bellocchi, Enrica Bunker, Andrew Campbell, Steph Combes, Françoise Davies, Richard Diaz-Santos, Tanio Fuller, Lindsay Gandhi, Poshak García-Burillo, Santiago González-Martín, Omaira Hicks, Erin K. S. Hönig, Sebastian Ichikawa, Kohei Imanishi, Masatoshi Izumi, Takuma Labiano, Alvaro Levenson, Nancy A. Packham, Christopher Rosario, David Rigopoulou, Dimitra Rouan, Daniel Shimizu, Taro Stalevski, Marko Ward, Martin Zhang, Lulu Ricci, Claudio Esparza-Arredondo, Donaji García-Lorenzo, Begoña |
| author_facet | Lopez-Rodriguez, Enrique Almeida, Cristina Ramos Pereira-Santaella, Miguel García-Bernete, Ismael Nikutta, Robert Alonso-Herrero, Almudena Bellocchi, Enrica Bunker, Andrew Campbell, Steph Combes, Françoise Davies, Richard Diaz-Santos, Tanio Fuller, Lindsay Gandhi, Poshak García-Burillo, Santiago González-Martín, Omaira Hicks, Erin K. S. Hönig, Sebastian Ichikawa, Kohei Imanishi, Masatoshi Izumi, Takuma Labiano, Alvaro Levenson, Nancy A. Packham, Christopher Rosario, David Rigopoulou, Dimitra Rouan, Daniel Shimizu, Taro Stalevski, Marko Ward, Martin Zhang, Lulu Ricci, Claudio Esparza-Arredondo, Donaji García-Lorenzo, Begoña |
| contents | The polar mid-infrared (MIR) emission detected within 10-100s pcs 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/MIRI imaging observations with 7-25 $μ$m JWST/MRS integral field spectroscopic observations of 6 nearby, $\bar{D}=35.4\pm4.6$ 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, $\log_{10}(\bar{L}_{bol}\,[erg\,s^{-1}])=44.0\pm0.3$, span a wide range of optical outflow rates, $\dot{M}=0.003-0.21$ M$_{\odot}$ yr$^{-1}$, column densities, $\log_{10}(N_{H}^{X-ray}[cm^{-2}])=22.2-24.3$, 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, $T_{d}=132^{+7}_{-7}$ K, and mass, $M_{d}=728^{+29}_{-27}$ M$_{\odot}$. Using the conditions of energy balance between radiation-pressure and gravity ($λ_{Edd}$ vs. N$_{H}$), we find that our AGN sample is in the gravitationally bounded regime consistent with no detection of dusty winds. At 10 $μ$m, the level of extended line emission contribution is correlated with the outflow kinetic energy and mass outflow rates. We find no correlation with the AGN properties. These results indicate that the radio jet may be triggering the gas outflow and line emission, while the extended dust emission is distributed in molecular clouds and/or shocked regions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_19350 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | GATOS. VIII. On the physical origin of the extended MIR emission in AGN Lopez-Rodriguez, Enrique Almeida, Cristina Ramos Pereira-Santaella, Miguel García-Bernete, Ismael Nikutta, Robert Alonso-Herrero, Almudena Bellocchi, Enrica Bunker, Andrew Campbell, Steph Combes, Françoise Davies, Richard Diaz-Santos, Tanio Fuller, Lindsay Gandhi, Poshak García-Burillo, Santiago González-Martín, Omaira Hicks, Erin K. S. Hönig, Sebastian Ichikawa, Kohei Imanishi, Masatoshi Izumi, Takuma Labiano, Alvaro Levenson, Nancy A. Packham, Christopher Rosario, David Rigopoulou, Dimitra Rouan, Daniel Shimizu, Taro Stalevski, Marko Ward, Martin Zhang, Lulu Ricci, Claudio Esparza-Arredondo, Donaji García-Lorenzo, Begoña Astrophysics of Galaxies The polar mid-infrared (MIR) emission detected within 10-100s pcs 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/MIRI imaging observations with 7-25 $μ$m JWST/MRS integral field spectroscopic observations of 6 nearby, $\bar{D}=35.4\pm4.6$ 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, $\log_{10}(\bar{L}_{bol}\,[erg\,s^{-1}])=44.0\pm0.3$, span a wide range of optical outflow rates, $\dot{M}=0.003-0.21$ M$_{\odot}$ yr$^{-1}$, column densities, $\log_{10}(N_{H}^{X-ray}[cm^{-2}])=22.2-24.3$, 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, $T_{d}=132^{+7}_{-7}$ K, and mass, $M_{d}=728^{+29}_{-27}$ M$_{\odot}$. Using the conditions of energy balance between radiation-pressure and gravity ($λ_{Edd}$ vs. N$_{H}$), we find that our AGN sample is in the gravitationally bounded regime consistent with no detection of dusty winds. At 10 $μ$m, the level of extended line emission contribution is correlated with the outflow kinetic energy and mass outflow rates. We find no correlation with the AGN properties. These results indicate that the radio jet may be triggering the gas outflow and line emission, while the extended dust emission is distributed in molecular clouds and/or shocked regions. |
| title | GATOS. VIII. On the physical origin of the extended MIR emission in AGN |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2507.19350 |