The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105

• Published in: The Astrophysical journal 2023-12, Vol.959 (2), p.107
• Main Authors: Singha, M., Winkel, N., Vaddi, S., Perez Torres, M., Gaspari, M., Smirnova-Pinchukova, I., O’Dea, C. P., Combes, F., Omoruyi, Osase, Rose, T., McElroy, R., Husemann, B., Davis, T. A., Baum, S. A., Lawlor-Forsyth, C., Neumann, J., Tremblay, G. R.
• Format: Article
• Language: English
• Subjects: Active galactic nuclei; AGN host galaxies; Astrophysics; Black holes; Continuum radiation; Deposition; Emissions; Field cameras; Galaxies; Galaxy evolution; Hubble Space Telescope; Interstellar matter; Interstellar medium; Ionization; Kinematics; Luminosity; Morphology; Outflow; Quasars; Radiation; Radiation pressure; Radio emission; Radio jets; Radio jets (astronomy); Space telescopes; Star & galaxy formation; Star formation; Stellar coronas; Very Large Telescope
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad004d

We present a case study of HE 0040-1105, an unobscured radio-quiet active galactic nucleus (AGN) at a high accretion rate of λ Edd = 0.19 ± 0.04. This particular AGN hosts an ionized gas outflow with the largest spatial offset from its nucleus compared to all other AGNs in the Close AGN Reference Survey. By combining multiwavelength observations from the Very Large Telescope/MUSE, Hubble Space Telescope/Wide Field Camera 3, Very Large Array, and European VLBI Network, we probe the ionization conditions, gas kinematics, and radio emission from host galaxy scales to the central few parsecs. We detect four kinematically distinct components, one of which is a spatially unresolved AGN-driven outflow located within the central 500 pc, where it locally dominates the interstellar medium conditions. Its velocity is too low to escape the host galaxy’s gravitational potential, and may be re-accreted onto the central black hole via chaotic cold accretion. We detect compact radio emission in HE 0040-1105 within the region covered by the outflow, varying on a timescale of ∼20 yr. We show that neither AGN coronal emission nor star formation processes wholly explain the radio morphology/spectrum. The spatial alignment between the outflowing ionized gas and the radio continuum emission on 100 pc scales is consistent with a weak jet morphology rather than diffuse radio emission produced by AGN winds. >90% of the outflowing ionized gas emission originates from the central 100 pc, within which the ionizing luminosity of the outflow is comparable to the mechanical power of the radio jet. Although radio jets might primarily drive the outflow in HE 0040-1105, radiation pressure from the AGN may contribute to this process.