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dc.rights.license© ESO 2020-
dc.contributor.authorFernández Ontiveros, J. A.-
dc.contributor.authorDasyra, K. M.-
dc.contributor.authorHatziminaoglou, Evanthia-
dc.contributor.authorMalkan, M. A.-
dc.contributor.authorPereira Santaella, M.-
dc.contributor.authorPapachristou, M.-
dc.contributor.authorSpinoglio, L.-
dc.contributor.authorCombes, F.-
dc.contributor.authorAalto, S.-
dc.contributor.authorNagar, N.-
dc.contributor.authorImanishi, M.-
dc.contributor.authorAndreani, P.-
dc.contributor.authorRicci, C.-
dc.contributor.authorSlater, R.-
dc.contributor.otherUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737-
dc.identifier.citationAstronomy and Astrophysics 633: A127(2020)es
dc.description.abstractA prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of 340-600 pc from the nucleus. The wind morphology resembles the characteristic funnel shape, formed by a highly collimated filamentary emission at the base, and likely traces the jet propagation through a tenuous medium, until a bifurcation point at 440 pc. Here the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner less than or similar to 340 pc using the [NeII](12.8 mu m) line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of similar to 8 x 10(6) M-circle dot at an average wind projected speed of similar to 160 km s(-1), which implies a mass outflow rate of similar to 14 M-circle dot yr(-1). Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where a previously unknown jet is revealed through its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain an outflow at this distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the
dc.description.sponsorshipThe authors acknowledge the referee for his/her useful comments that helped to improve the manuscript. JAFO acknowledges financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. JAFO and KMD acknowledge financial support by the Hellenic Foundation for Research and Innovation (HFRI), under the first call for the creation of research groups by postdoctoral researchers that was launched by the General Secretariat For Research and Technology (project number 1882). MPS acknowledges support from the Comunidad de Madrid, Spain, through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and STFC through grants ST/N000919/1 and ST/N002717/1. CR acknowledges support from the CONI-CYT +PAI, Convocatoria Nacional subvencion a instalacion en la academia, convocatoria ano 2017 PAI77170080. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.00236.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).es
dc.publisherEDP Scienceses
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 International*
dc.subjectISM: jets and outflowses
dc.subjectGalaxies: activees
dc.subjectGalaxies: individuales
dc.subjectESO 420-G13es
dc.subjectSubmillimeter: ISMes
dc.subjectGalaxies: evolutiones
dc.subjectTechniques: high angular resolutiones
dc.titleA CO molecular gas wind 340 pc away from the Seyfert 2 nucleus in ESO 420-G13 probes an elusive radio jetes
dc.contributor.orcidFernández Ontiveros, J. A. [0000-0001-9490-899X]-
dc.contributor.orcidHatziminaoglou, E. [0000-0003-0917-9636]-
dc.contributor.orcidSpignoglio, L. [0000-0001-8840-1551]-
dc.contributor.orcidCombes, F. [0000-0003-2658-7893]-
dc.contributor.orcidNagar, N. [0000-0001-6920-662X]-
dc.contributor.orcidImanishi, M. [0000-0001-6186-8792]-
dc.contributor.orcidAndreani, P. [0000-0001-9493-0169]-
dc.contributor.funderAgenzia Spaziale Italiana (ASI)-
dc.contributor.funderComunidad de Madrid-
dc.contributor.funderHellenic Foundation for Research and Innovation (HFRI)-
dc.contributor.funderComisión Nacional de Investigación Científica y Tecnológica (CONICYT)-
dc.description.peerreviewedPeer reviewes
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