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Lookup NU author(s): Dr David Rosario
This work is licensed under a Creative Commons Attribution 4.0 International License (CC BY 4.0).
© 2023 AuthorsWe present a spatially resolved study of the ionized gas in the central 2 kpc of the Seyfert 2 galaxy NGC 2110 and investigate the role of its moderate-luminosity radio jet (kinetic radio power of Pjet=2.3 - 1043 erg s-1). We used new optical integral-field observations taken with the MEGARA spectrograph at the Gran Telescopio Canarias, which cover the 4300 -5200 and 6100 -7300 ranges with a spectral resolution of Ra5000 - 5900. We fitted the emission lines with a maximum of two Gaussian components, except at the position of the active galactic nucleus (AGN), where we used three. Aided by existing stellar kinematics, we used the observed velocity and velocity dispersion (σ) of the emission lines to classify the different kinematic components. The disk component is characterized by lines with σ a60 - 200 km s-1. The outflow component has typical values of σ a700 km s-1 and is confined to the central 2.5 a400 pc, which is coincident with the linear part of the radio jet detected in NGC 2110. At the AGN position, the [O III]λ5007 line shows high velocity components that reach at least 1000 km s-1. This and the high velocity dispersions indicate the presence of outflowing gas outside the galaxy plane. Spatially resolved diagnostic diagrams reveal mostly low ionization (nuclear) emitting region-like excitation in the outflow and some regions in the disk, which could be due to the presence of shocks. However, there is also Seyfert-like excitation beyond the bending of the radio jet, which probably traces the edge of the ionization cone that intercepts with the disk of the galaxy. NGC 2110 follows the observational trends between the outflow properties and the jet radio power found for a few nearby Seyfert galaxies. All these pieces of information suggest that part of the observed ionized outflow in NGC 2110 might be driven by the radio jet. However, the radio jet was bent at radial distances of 200 pc (in projection) from the AGN, and beyond there, most of the gas in the galaxy disk is rotating.
Author(s): Peralta De Arriba L, Alonso-Herrero A, Garcia-Burillo S, Garcia-Bernete I, Villar-Martin M, Garcia-Lorenzo B, Davies R, Rosario DJ, Honig SF, Levenson NA, Packham C, Ramos Almeida C, Pereira-Santaella M, Audibert A, Bellocchi E, Hicks EKS, Labiano A, Ricci C, Rigopoulou D
Publication type: Article
Publication status: Published
Journal: Astronomy and Astrophysics
Year: 2023
Volume: 675
Print publication date: 01/07/2023
Online publication date: 30/06/2023
Acceptance date: 08/05/2023
Date deposited: 25/07/2023
ISSN (print): 0004-6361
ISSN (electronic): 1432-0746
Publisher: EDP Sciences
URL: https://doi.org/10.1051/0004-6361/202245408
DOI: 10.1051/0004-6361/202245408
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