Gas-phase metallicity determinations in nearby AGNs with SDSS-IV MaNGA : evidence of metal-poor accretion

• Autor(a) principal: Nascimento, Janaina Correa do
• Data de Publicação: 2022
• Outros Autores: Dors Júnior, Oli Luiz, Storchi-Bergmann, Thaisa, Mallmann, Nícolas Dullius, Riffel, Rogério, Ilha, Gabriele da Silva, Riffel, Rogemar André, Rembold, Sandro Barboza, Machado, Alice Deconto, Costa, Luiz N. da, Armah, Mark
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/239505
• topic: Galáxias ativas; Metalicidade; Evolucao galatica; Cinemática; Galaxies : Abundances; Galaxies : Active; Galaxies : Evolution

We derive the metallicity (traced by the O/H abundance) of the narrow-line region (NLR) of 108 Seyfert galaxies as well as radial metallicity gradients along their galaxy discs and of these of a matched control sample of no active galaxies. In view of that, observational data from the SDSS-IV MaNGA survey and strong emission-line calibrations taken from the literature were considered. The metallicity obtained for the NLRs was compared to the value derived from the extrapolation of the radial oxygen abundance gradient, obtained from H II region estimates along the galaxy disc, to the central part of the host galaxies. We find that, for most of the objects (∼ 80 per cent), the NLR metallicity is lower than the extrapolated value, with the average difference ( D ) between these estimates ranging from 0.16 to 0.30 dex. We suggest that D is due to the accretion of metal-poor gas to the AGN that feeds the nuclear supermassive black hole (SMBH), which is drawn from a reservoir molecular and/or neutral hydrogen around the SMBH. Additionally, we look for correlations between D and the electron density (Ne), [O III]λ5007, and H α luminosities, extinction coefficient (AV) of the NLRs, as well as the stellar mass (M∗) of the host galaxies. Evidence of an inverse correlation between the D and the parameters Ne, M∗, and Av was found.