An outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observations

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dc.contributor.authorHumire, P.K.
dc.contributor.authorNagar, N.M.
dc.contributor.authorFinlez, C.
dc.contributor.authorFirpo, V.
dc.contributor.authorSlater, R.
dc.contributor.authorLena, D.
dc.contributor.authorSoto-Pinto, P.
dc.contributor.authorMuñoz-Vergara, D.
dc.contributor.authorRiffel, R.A.
dc.contributor.authorSchmitt, H.R.
dc.contributor.authorKraemer, S.B.
dc.contributor.authorSchnorr-Müller, A.
dc.contributor.authorFischer, T.C.
dc.contributor.authorRobinson, A.
dc.contributor.authorStorchi-Bergmann, T.
dc.contributor.authorCrenshaw, M.
dc.contributor.authorElvis, M.S.
dc.date.accessioned2019-10-28T13:52:46Z
dc.date.available2019-10-28T13:52:46Z
dc.date.issued2018
dc.descriptionIndexación: Scopus.es
dc.description.abstractWe present two-dimensional stellar and gaseous kinematics of the inner 0.7 × 1.2 kpc2 of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092-7338 Å) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of ≈ 170 pc and spectral resolution of 36 km s-1. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [O III] emission shows a fan-shaped extension of ≈ 10′′ to the SE. We detect the [O III] doublet, [N II] and Hα emission lines throughout our field of view. The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ≈ 137° and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122° to 139°, projected velocity amplitudes of the order of 100 km s-1, and a mean velocity dispersion of 100 km s-1. A double-Gaussian fit to the [O III]λ5007 and Hα lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight velocities 100-250 km s-1 higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4 × 10-2 M⊙ yr-1 in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2 × 10-2 M⊙ yr-1. The total ionized gas mass within ∼84 pc of the nucleus is 3.3 × 105 M⊙; infall velocities of ∼34 km s-1 in this gas would be required to feed both the outflow and SMBH accretion. © ESO 2018.es
dc.description.urihttps://www.aanda.org/articles/aa/abs/2018/06/aa31671-17/aa31671-17.html
dc.identifier.citationAstronomy and Astrophysics, 614, art. no. A94es
dc.identifier.issn0004-6361
dc.identifier.other10.1051/0004-6361/201731671
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/10558
dc.language.isoenes
dc.publisherEDP Scienceses
dc.subjectGalaxies: activees
dc.subjectGalaxies: individual: ESO 362-G18es
dc.subjectGalaxies: kinematics and dynamicses
dc.subjectGalaxies: nucleies
dc.subjectGalaxies: Seyfertes
dc.titleAn outflow in the Seyfert ESO 362-G18 revealed by Gemini-GMOS/IFU observationses
dc.typeArtículoes
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