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dc.contributor.authorSoto-Pinto, Pamelapt_BR
dc.contributor.authorNagar, Neil M.pt_BR
dc.contributor.authorFinlez, Carolinapt_BR
dc.contributor.authorRamakrishnan, Venkatesshpt_BR
dc.contributor.authorMunõz-Vergara, Daniapt_BR
dc.contributor.authorSlater, Roypt_BR
dc.contributor.authorHumire, Pedro K.pt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorLena, Davidept_BR
dc.contributor.authorKraemer, S. B.pt_BR
dc.contributor.authorFischer, Travis C.pt_BR
dc.contributor.authorSchmitt, Henrique Robertopt_BR
dc.contributor.authorRiffel, Rogemar Andrépt_BR
dc.contributor.authorSchnorr Müller, Allanpt_BR
dc.contributor.authorRobinson, Andrewpt_BR
dc.contributor.authorCrenshaw, Daniel Michaelpt_BR
dc.contributor.authorElvis, Martinpt_BR
dc.date.accessioned2019-12-27T04:02:09Zpt_BR
dc.date.issued2019pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/203749pt_BR
dc.description.abstractWe present two-dimensional ionized gas and stellar kinematics in the inner 1.4 × 1.9 kpc2 of the Seyfert 2 galaxy ESO 153-G20 obtained with the Gemini-South/Gemini multi-object spectrograph integral field unit (GMOS-IFU) at a spatial resolution of ~250 pc and spectral resolution of 36 km s−1. Strong [O iii], Hα, [N ii] and [S ii] emission lines are detected over the entire field of view. The stellar kinematics trace circular rotation with a projected velocity amplitude of ±96 km s−1, a kinematic major axis in position angle of 11°, and an average velocity dispersion of 123 km s−1. To analyse the gas kinematics, we used aperture spectra, position–velocity diagrams and single/double Gaussian fits to the emission lines. All lines show two clear kinematic components: a rotating component that follows the stellar kinematics, and a larger-dispersion component, close to the systemic velocity (from which most of the [O iii] emission comes), mainly detected to the south-west. We interpret this second component as gas outflowing at ~400 km s−1 in a compact (300 pc) ionization cone with a half-opening angle ≤40°. The counter-cone is probably obscured behind a dust lane. We estimate a mass outflow rate of 1.1 M⊙ yr−1, 200 times larger than the estimated accretion rate on to the supermassive black hole, and a kinetic to radiative power ratio of 1.7 × 10−3. Bar-induced perturbations probably explain the remaining disturbances observed in the velocity field of the rotating gas component.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 489, no. 3 (Sep. 2019), p. 4111-4124pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxias seyfertpt_BR
dc.subjectGalaxies: activeen
dc.subjectGalaxies: individual : ESO 153-G20en
dc.subjectFormacao de estrelaspt_BR
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectGaláxias ativaspt_BR
dc.subjectGalaxies: nucleien
dc.subjectGalaxies: Seyferten
dc.titleOutflowing gas in a compact ionization cone in the Seyfert 2 galaxy ESO 153-G20pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001105730pt_BR
dc.type.originEstrangeiropt_BR


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