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dc.contributor.authorSales, Dinalva Aires dept_BR
dc.contributor.authorRobinson, Andrewpt_BR
dc.contributor.authorRiffel, Rogemar Andrépt_BR
dc.contributor.authorStorchi-Bergmann, Thaisapt_BR
dc.contributor.authorGallimore, Jack F.pt_BR
dc.contributor.authorKharb, Preetipt_BR
dc.contributor.authorBaum, Stefi Alisonpt_BR
dc.contributor.authorO’Dea, Christopherpt_BR
dc.contributor.authorCarpes, Hekatelyne Prestespt_BR
dc.contributor.authorFerrari, Fabriciopt_BR
dc.date.accessioned2019-08-28T02:34:18Zpt_BR
dc.date.issued2019pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/198447pt_BR
dc.description.abstractWe present a multiwavelength study of the OH megamaser galaxy IRAS17526 + 3253, based on new Gemini multi-object spectrograph integral field unit (GMOS/IFU) observations, Hubble Space Telescope F814W, and H α + [N II] images, and archival 2MASS and 1.49 GHz VLA data. The Hubble Space Telescope (HST) images clearly reveal a mid-to-advanced stage major merger whose northwestern and southeastern nuclei have a projected separation of ∼8.5 kpc. Our HST/H α + [N II] image shows regions of ongoing star formation across the envelope on∼10 kpc scales, which are aligned with radio features, supporting the interpretation that the radio emission originates from star-forming regions. The measured H α luminosities imply that the unobscured star formation rate (SFR) is ∼10–30 M yr−1. The GMOS/IFU data reveal two structures in northwestern separated by 850 pc and by a discontinuity in the velocity field of ∼ 200 km s−1. We associate the blueshifted and redshifted components with, respectively, the distorted disc of northwestern and tidal debris, possibly a tail originating in southeastern. Star formation is the main ionization source in both components, which have SFRs of ∼2.6–7.9 M yr−1 and ∼1.5–4.5 M yr−1, respectively. Fainter line emission bordering these main components is consistent with shock ionization at a velocity ∼200 km s−1 and may be the result of an interaction between the tidal tail and the northwestern galaxy’s disc. IRAS17526 + 3253 is one of only a few systems known to host both luminous OH and H2O masers. The velocities of the OH and H2O maser lines suggest that they are associated with the northwestern and southeastern galaxies, respectively (Martin et al.; Wagner).en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 486, no. 3 (July 2019), p. 3350-3367pt_BR
dc.rightsOpen Accessen
dc.subjectGaláxias ativaspt_BR
dc.subjectTechniques: spectroscopicen
dc.subjectGalaxies: activeen
dc.subjectEvolucao galaticapt_BR
dc.subjectGalaxies: evolutionen
dc.subjectCinemática estelarpt_BR
dc.subjectGalaxies: individual: IRAS17526 + 3253en
dc.subjectGalaxies: interactionsen
dc.titleGemini IFU, VLA, and HST observations of the OH Megamaser Galaxy IRAS17526 + 3253pt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001098845pt_BR
dc.type.originEstrangeiropt_BR


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