A radio-jet-driven outflow in the Seyfert 2 galaxy NGC 2110?

¹ Centro de Astrobiología (CAB), CSIC-INTA, Camino Bajo del Castillo s/n, 28692 Villanueva de la Cañada, Madrid, Spain
e-mail: lperalta@cab.inta-csic.es; aalonso@cab.inta-csic.es
² Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, 28014 Madrid, Spain
³ Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH UK
⁴ Centro de Astrobiología (CAB), CSIC-INTA, Carretera de Ajalvir km 4, 28850 Torrejón de Ardoz, Madrid, Spain
⁵ Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea, s/n, 38205 La Laguna, Tenerife, Spain
⁶ Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
⁷ Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
⁸ School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne, NE1 7RU UK
⁹ School of Physics & Astronomy, University of Southampton, Southampton, SO17 1BJ Hampshire, UK
¹⁰ Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD, 21218 USA
¹¹ The University of Texas at San Antonio, 1 UTSA Circle, San Antonio, TX, 78249 USA
¹² National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS), 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 Japan
¹³ Instituto de Física Fundamental, CSIC, Calle Serrano 123, 28006 Madrid, Spain
¹⁴ Departamento de Física de la Tierra y Astrofísica, Fac. de CC Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain
¹⁵ Instituto de Física de Partículas y del Cosmos IPARCOS, Fac. CC Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain
¹⁶ Department of Physics & Astronomy, University of Alaska Anchorage, Anchorage, AK, 99508-4664 USA
¹⁷ Telespazio UK for the European Space Agency, ESAC, Camino Bajo del Castillo s/n, 28692 Villanueva de la Cañada, Spain
¹⁸ Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile
¹⁹ Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, 100871 PR China
²⁰ School of Sciences, European University Cyprus, Diogenes Street, Engomi, 1516 Nicosia, Cyprus

Received: 8 November 2022
Accepted: 8 May 2023

Abstract

We 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 P_jet = 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 Å and 6100 − 7300 Å ranges with a spectral resolution of R ≃ 5000 − 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 ≃ 60 − 200 km s⁻¹. The outflow component has typical values of σ ≃ 700 km s⁻¹ and is confined to the central 2.5″ ≃ 400 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.