Publicación Artículo científico (article).

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

Digital.CSIC. Repositorio Institucional del CSIC
Digital.CSIC. Repositorio Institucional del CSIC
  • Peralta de Arriba, L.
  • Alonso-Herrero, A.
  • García-Burillo. S.
  • García-Bernete, I.
  • Villar-Martín, M.
  • García-Lorenzo, B.
  • Davies, R.
  • Rosario, D. J.
  • Hönig, S. F.
  • Levenson, N. A.
  • Packham, C.
  • Ramos Almeida, C.
  • Pereira-Santaella, Miguel
  • Audibert, A.
  • Bellocchi, E.
  • Hicks, E. K. S.
  • Labiano, A.
  • Ricci, C.
  • Rigopoulou, D.
25 pages, 22 figures, 3 tables, We present a spatially-resolved study of the ionised 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 $P_\mathrm{jet} = 2.3 \times 10^{43}\mathrm{erg\ s^{-1}}$). We use new optical integral-field observations taken with the MEGARA spectrograph at GTC. We fit the emission lines with a maximum of two Gaussian components, except at the AGN position where we used three. Aided by existing stellar kinematics, we use the observed velocity and velocity dispersion of the emission lines to classify the different kinematic components. The disc component is characterised by lines with $\sigma \sim 60-200\ \mathrm{km\ s^{-1}}$. The outflow component has typical values of $\sigma \sim 700\ \mathrm{km\ s^{-1}}$ and is confined to the central 400 pc, which is coincident with linear part of the radio jet detected in NGC 2110. At the AGN position, the [O III]$\lambda$5007 line shows high velocity components reaching at least $1000\ \mathrm{km\ s^{-1}}$. This and the high velocity dispersions indicate the presence of outflowing gas outside the galaxy plane. Spatially-resolved diagnostic diagrams reveal mostly LI(N)ER-like excitation in the outflow and some regions in the disc, which could be due to the presence of shocks. However, there is also Seyfert-like excitation beyond the bending of the radio jet, probably tracing the edge of the ionisation cone that intercepts with the disc of the galaxy. NGC 2110 follows well 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 observed ionised 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 disc is rotating., L.P.d.A., A.A.H., S.G.B., and M.V.M. acknowledge financial support from grant PGC2018-094671-B-I00 funded by MCIN/AEI/10.13039/501100011033 and by ERDF A way of making Europe. A.A.H. and M.V.M. also acknowledge financial support from grant PID2021-124665NB-I00 funded by the Spanish Ministry of Science and Innovation and the State Agency of Research MCIN/AEI/ 10.13039/501100011033 and ERDF A way of making Europe. S.G.B. acknowledges support from the research project PID2019-106027GAC44 of the Spanish Ministerio de Ciencia e Innovación. I.G.B. and D.R. acknowledge support from STFC through grant ST/S000488/1. B.G.L. acknowledges support from grants PID2019-107010GB-100 and the Severo Ochoa CEX2019-000920-S. C.R.A. acknowledges the project “Feeding and feedback in active galaxies”, with reference PID2019-106027GB-C42, funded by MICINNAEI/10.13039/501100011033, and the European Union’s Horizon 2020 research and innovation programme under Marie Skłodowska-Curie grant agreement No 860744 (BID4BEST). C.R.A. and A.A. acknowledge the project “Quantifying the impact of quasar feedback on galaxy evolution”, with reference EUR2020-112266, funded by MICINN-AEI/10.13039/501100011033 and the European Union NextGenerationEU/PRTR; the Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant “Quasar feedback and molecular gas reservoirs”, with reference ProID2020010105, ACCISI/FEDER, UE. E.B. acknowledges the María Zambrano program of the Spanish Ministerio de Universidades funded by the Next Generation European Union and is also partly supported by grant RTI2018-096188-B-I00 funded by MCIN/AEI/10.13039/501100011033. C.R. acknowledges support from the Fondecyt Iniciacion grant 11190831 and ANID BASAL project FB210003. D.R. acknowledges support from University of Oxford John Fell Fund., Peer reviewed

Digital.CSIC. Repositorio Institucional del CSIC

Digital.CSIC. Repositorio Institucional del CSIC
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Digital.CSIC. Repositorio Institucional del CSIC