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dc.contributor.authorMunõz-Vergara, Daniapt_BR
dc.contributor.authorNagar, Neil M.pt_BR
dc.contributor.authorRamakrishnan, Venkatesshpt_BR
dc.contributor.authorFinlez, Carolinapt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorSlater, Roypt_BR
dc.contributor.authorFirpo, Verónicapt_BR
dc.contributor.authorHumire, Pedro K.pt_BR
dc.contributor.authorSoto-Pinto, Pamelapt_BR
dc.contributor.authorKraemer, S. B.pt_BR
dc.contributor.authorLena, Davidept_BR
dc.contributor.authorRobinson, Andrewpt_BR
dc.contributor.authorRiffel, Rogemar Andrépt_BR
dc.contributor.authorCrenshaw, Daniel Michaelpt_BR
dc.contributor.authorElvis, Martinpt_BR
dc.contributor.authorFischer, Travis C.pt_BR
dc.contributor.authorSchnorr Müller, Allanpt_BR
dc.contributor.authorSchmitt, Henrique Robertopt_BR
dc.date.accessioned2019-09-12T03:41:49Zpt_BR
dc.date.issued2019pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/199111pt_BR
dc.description.abstractAs part of a high-resolution observational study of feeding and feedback processes occurring in the vicinity of the active galactic nucleus in 40 galaxies, we observed the inner 3′′.5 × 5 arcsec of the nearby spiral and Seyfert 2 galaxy UGC 2024 with the integral field unit of the Gemini-South Telescope. The observations enabled a study of the stellar and gas kinematics in this region at a spatial resolution of 0′′.5 (218 pc), and a spectral resolution of 36  km s−1 over the wavelength range 4100–7300 Å. For the strongest emission-lines (H β, [OIII] λ5007 Å, H α, [NII] λ6584 Å, and [SII] λλ6717,6731 Å) we derived maps of the flux, radial velocity, and velocity dispersion. The flux distribution and kinematics of the [OIII] emission line are roughly symmetric around the nucleus: the radial velocity is close to systemic over the full field of view. The kinematics of the other strong emission lines trace both this systemic velocity component, and ordered rotation (with kinematic centre 0′′.2 north-west of the nucleus). The stellar continuum morphology and kinematics are, however, asymmetrical around the nucleus. We interpret these unusual kinematics as the superposition of a component of gas rotating in the galaxy disc plus a ‘halo’ component of highly ionized gas. This halo either traces a quasi-spherical fountain with average radial velocity 200 km s−1, in which case the total nuclear outflow mass and momentum are 2 × 105 M⊙ and 4 × 107 M⊙ km s−1, respectively, or a dispersion supported halo created by a past nuclear starbursten
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 487, no. 3 (Aug. 2019), p. 3679-3692pt_BR
dc.rightsOpen Accessen
dc.subjectGalaxies: activeen
dc.subjectGalaxias seyfertpt_BR
dc.subjectGalaxies: individualen
dc.subjectEvolucao galaticapt_BR
dc.subjectUGC 2024en
dc.subjectGaláxias ativaspt_BR
dc.subjectgalaxies: kinematics and dynamicsen
dc.subjectgalaxies: nucleien
dc.subjectGalaxies: Seyferten
dc.titleA nuclear ionized gas outflow in the Seyfert 2 galaxy UGC 2024pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001100088pt_BR
dc.type.originEstrangeiropt_BR


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