Evidence of galaxy interaction in the Narrow-line Seyfert 1 galaxy IRAS17020+4544 seen by NOEMA

The narrow-line Seyfert 1 galaxy IRAS17020+4544 is one of the few sources where both an X-ray ultra-fast outflow and a molecular outflow were observed to be consistent with energy conservation. However, IRAS17020+4544 is less massive and has a much more modest active galactic nucleus (AGN) luminosity than the other examples. Using recent CO(1-0) observations with the NOrthern Extended Millimeter Array (NOEMA), we characterised the molecular gas content of the host galaxy for the first time. We found that the molecular gas is distributed into an apparent central disc of 1.1x10^9 Msun, and a northern extension located up to 8 kpc from the centre with a molecular gas mass M_H2~10^8 Msun. The molecular gas mass and the CO dynamics in the northern extension reveal that IRAS 17020+4544 is not a standard spiral galaxy, instead it is interacting with a dwarf object corresponding to the northern extension. This interaction possibly triggers the high accretion rate onto the super massive black hole. Within the main galaxy, which hosts the AGN, a simple analytical model predicts that the molecular gas may lie in a ring, with less molecular gas in the nuclear region. Such distribution may be the result of the AGN activity which removes or photodissociates the molecular gas in the nuclear region (AGN feedback). Finally, we have detected a molecular outflow of mass M_H2=(0.7-1.2)x10^7 Msun in projection at the location of the northern galaxy, with a similar velocity to that of the massive outflow reported in previous millimeter data obtained by the Large Millimeter Telescope.Comment: Published in MNRAS, Volume 501, Issue 1, Pages 219-22

MUSE reveals extended circumnuclear outflows in the seyfert 1 NGC 7469

NGC 7469 is a well-known luminous infrared galaxy, with a circumnuclear star formation ring ∼830 pc radius) surrounding a Seyfert 1 active galactic nucleus (AGN). Nuclear unresolved winds were previously detected in X-rays and ultraviolet, as well as an extended biconical outflow in infrared coronal lines. We search for extended outflows by measuring the kinematics of the Hβ and [O III] λ5007 optical emission lines, in data of the Very Large Telescope/Multi-unit Spectroscopic Explorer integral field spectrograph. We find evidence of two outflow kinematic regimes: One slower regime extending across most of the star formation (SF) ring-possibly driven by the massive SF-and a faster regime (with a maximum velocity of -715 km s-1), only observed in [O III], in the western region between the AGN and the massive star-forming regions of the ring, likely AGN-driven. This work shows a case where combined AGN/SF feedback can be effectively spatially resolved, opening up a promising path toward a deeper understanding of feedback processes in the central kiloparsec of AGNSupport from CONACyT (Mexico) grant CB-2016-01-286316 is acknowledged. J.P.T.P. acknowledges DAIP-UGto (Mexico) for granted support (0173/2019). Y.A. acknowledges support from project PID2019-107408GB-C42 (Ministerio de Ciencia e Innovación, Spain). S.F.S. thanks the support of CONACYT grants CB-285080 and FC-2016-01- 1916, and funding from the PAPIIT-DGAPA-IN100519 (UNAM) project. L.G. was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). E.B acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. This research has been partially funded by the Spanish State Research Agency (AEI) Project MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC

NOEMA spatially resolved view of the multiphase outflow in IRAS17020+4544: a shocked wind in action?

Funding Information: We are grateful to the anonymous referee for their careful review of the manuscript that significantly improved our publication. This work is based on observations carried out under project number W17CR with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This research has used data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application package ciao . The author is grateful to the Chandra-CXC Helpdesk and to H. Marshall and D. Huenemoerder for their support on the treatment of the HRC-LETG data. ALL and QS acknowledge support from CONACyT grant CB-2016-01-286316. ALL acknowledges support from DGAPA-PAPIIT grant IA101623. YK acknowledges support from DGAPA-PAPIIT grant IN106518 and 102023. VMPA and VC acknowledge support from CONACyT research grants 280789 and 320987. C.F. acknowledges support from the PRIN MIUR project “Black hole winds and the baryon life cycle of galaxies: the stone-guest at the galaxy evolution supper”, contract 2017PH3WAT.This work is supported by the MPIfR-Mexico Max Planck Partner Group led by V.M.P.-A. SGB acknowledges support from the research project PID2019-106027GA-C44 of the Spanish Ministerio de Ciencia e Innovación. ALL acknowledges the staff of the European Space Astronomy Centre (ESAC, Madrid) for hosting her visit during which this work was partly finalized. Financial support is acknowledged from ESA through the Science Faculty – Funding reference ESA-SCI-SC-LE-123, and from project PID2019-107408GB-C41 by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/ 10.13039/501100011033. Funding Information: We are grateful to the anonymous referee for their careful review of the manuscript that significantly improved our publication. This work is based on observations carried out under project number W17CR with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This research has used data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. The author is grateful to the Chandra-CXC Helpdesk and to H. Marshall and D. Huenemoerder for their support on the treatment of the HRC-LETG data. ALL and QS acknowledge support from CONACyT grant CB-2016-01-286316. ALL acknowledges support from DGAPAPAPIIT grant IA101623. YK acknowledges support from DGAPAPAPIIT grant IN106518 and 102023. VMPA and VC acknowledge support from CONACyT research grants 280789 and 320987. C.F. acknowledges support from the PRIN MIUR project “Black hole winds and the baryon life cycle of galaxies: the stone-guest at the galaxy evolution supper”, contract 2017PH3WAT.This work is supported by the MPIfR-Mexico Max Planck Partner Group led by V.M.P.-A. SGB acknowledges support from the research project PID2019-106027GA-C44 of the Spanish Ministerio de Ciencia e Innovación.ALL acknowledges the staff of the European Space Astronomy Centre (ESAC, Madrid) for hosting her visit during which this work was partly finalized. Financial support is acknowledged from ESA through the Science Faculty – Funding reference ESA-SCI-SC-LE-123, and from project PID2019-107408GB-C41 by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/10.13039/501100011033. Publisher Copyright: © 2023 The Author(s).The Narrow Line Seyfert 1 Galaxy IRAS17020+4544 is one of the few active galactic nuclei (AGNs) where a galaxy-scale energy-conserving outflow was revealed. This paper reports on NOEMA observations addressed to constrain the spatial scale of the CO emission in outflow. The molecular outflowing gas is resolved in five components tracing approaching and receding gas, all located at a distance of 2–3 kpc on the west and east sides of the active nucleus. This high-velocity gas (up to vout = ±1900 km s-1) is not coincident with the rotation pattern of the CO gas in the host galaxy disc. The estimated mass outflow rate shows that with a global mass output of M·H2 = 139±20 M☉ yr-1, this powerful galaxy-scale outflow is consistent with the wind conserving its energy, and with a momentum rate boost of a factor of ∼30 compared to the momentum rate of the nuclear X-ray wind. Preliminary results from ancillary X-ray (Chandra) and radio images (e-MERLIN) are reported. While the nature of the radio source is not conclusive, the Chandra image may tentatively trace extended emission, as expected by an expanding bubble of hot X-ray gas. The outcome of the NOEMA analysis and of the past and ongoing publications dedicated to the description of the outflow multiband phenomenology in IRAS17020+4544 concur to provide compelling reasons to postulate that an outflow shocking with the galaxy interstellar medium is driving the multiphase wind in this peculiar AGN.Peer reviewe