TY - JOUR
T1 - The Galaxy Activity, Torus, and Outflow Survey (GATOS)
T2 - II. Torus and polar dust emission in nearby Seyfert galaxies
AU - Alonso-Herrero, A.
AU - García-Burillo, S.
AU - Hönig, S. F.
AU - García-Bernete, I.
AU - Ramos Almeida, C.
AU - González-Martín, O.
AU - López-Rodríguez, E.
AU - Boorman, P. G.
AU - Bunker, A. J.
AU - Burtscher, L.
AU - Combes, F.
AU - Davies, R.
AU - Díaz-Santos, T.
AU - Gandhi, P.
AU - García-Lorenzo, B.
AU - Hicks, E. K.S.
AU - Hunt, L. K.
AU - Ichikawa, K.
AU - Imanishi, M.
AU - Izumi, T.
AU - Labiano, A.
AU - Levenson, N. A.
AU - Packham, C.
AU - Pereira-Santaella, M.
AU - Ricci, C.
AU - Rigopoulou, D.
AU - Roche, P.
AU - Rosario, D. J.
AU - Rouan, D.
AU - Shimizu, T.
AU - Stalevski, M.
AU - Wada, K.
AU - Williamson, D.
N1 - Funding Information:
Development Fund (ERDF) under grant with reference ProID2020010105 and from IAC project P/301404, financed by the Ministry of Science and Innovation, through the State Budget and by the Canary Islands Department of Economy, Knowledge and Employment, through the Regional Budget of the Autonomous Community. OG-M acknowledges support from UNAM PAPIIT IN105720. AJB has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 Advanced Grant 789056 “First Galaxies”. AA-H and AJB acknowledge support from a Royal Society International Exchange Grant. BG-L acknowledges support from the Spanish Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación (AEI-MCINN) under grant with reference PID2019-107010GB-I00. TI is supported by Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. JP20K14531. AL acknowledges the support from Comunidad de Madrid through the Atracción de Talento Investigador Grant 2017-T1/TIC-5213, and PID2019-106280GB-I00 (MCIU/AEI/FEDER,UE). MPS acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). DR acknowledges support from the Oxford Fell Fund and STFC through grant ST/S000488/1. DJR acknowledges support from the STFC (ST/T000244/1). MS is supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia through the contract no. 451-03-9/2021-14/200002 and the Science Fund of the Republic of Serbia, PROMIS 6060916, BOWIE. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere. Based on observations obtained at the international Gemini Observatory, a program of NSF’s NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Min-isterio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciên-cia, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00082.S and #2018.1.00113.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018). IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.
Funding Information:
Acknowledgements. We thank D. Asmus, M. Villar-Martín, and M. Venanzi for interesting discussions. AA-H and SG-B acknowledge support through grant PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE). AA-H, AL, and MPS work was done under project No. MDM-2017-0737 Unidad de Excelen-cia “María de Maeztu” – Centro de Astrobiología (INTA-CSIC). SG-B thanks support from the research project PID2019-106027GA-C44 from the Spanish Ministerio de Ciencia e Innovación. SFH acknowledges support by the EU Horizon 2020 framework programme via the ERC Starting Grant DUST-IN-THE-WIND (ERC-2015-StG-677117). IGB acknowledges support from STFC through grant ST/S000488/1. CRA acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MCIU) under grant with reference RYC-2014-15779, from the European Union’s Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement No 860744 (BiD4BESt), from the State Research Agency (AEI-MCINN) of the Spanish MCIU under grants “Feeding and feedback in active galaxies” with reference PID2019-106027GB-C42 and “Quantifying the impact of quasar feedback on galaxy evolution (QSOFEED)” with reference EUR2020-112266. CRA also acknowledges support from the Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the European Regional
Publisher Copyright:
© 2021 ESO.
PY - 2021/8/1
Y1 - 2021/8/1
N2 - 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.
AB - 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.
KW - Galaxies: ISM
KW - Galaxies: Seyfert
KW - Infrared: galaxies
KW - Submillimeter: galaxies
UR - http://www.scopus.com/inward/record.url?scp=85113386814&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85113386814&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202141219
DO - 10.1051/0004-6361/202141219
M3 - Article
AN - SCOPUS:85113386814
VL - 652
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A99
ER -