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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Chemical abundances of Seyfert 2 AGNs - I. Comparing oxygen abundances from distinct methods using SDSS

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Dors, O. L. [1] ; Freitas-Lemes, P. [1] ; Amores, E. B. [2] ; Perez-Montero, E. [3] ; Cardaci, V, M. ; Hagele, G. F. [4, 5] ; Armah, M. [1] ; Krabbe, A. C. [1] ; Faundez-Abans, M. [6]
Total Authors: 9
[1] Univ Vale Paraiba, Av Shishima Hifumi 2911, BR-12244000 Sao Jose Dos Campos, SP - Brazil
[2] Univ Estadual Feira De Santana, Dept Fis, Av Transnordestina S-N, BR-44036900 Feira De Santana, BA - Brazil
[3] Inst Astrofis Andalucia, Camino Bajo Huetor S-N, Aptdo 3004, E-18080 Granada - Spain
[4] Cardaci, M., V, Inst Astrofis La Plata, Ave Centenario Paseo Bosque S-N, B1900FWA, La Plata - Argentina
[5] Cardaci, M., V, Univ Nacl La Plata, Fac Ciencias Astron & Geofis, Paseo Bosque S-N, RA-1900 La Plata - Argentina
[6] Lab Nacl Astrofis, MCTIC, BR-37504364 Itajuba, MG - Brazil
Total Affiliations: 6
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 492, n. 1, p. 468-479, FEB 2020.
Web of Science Citations: 0

We compare the oxygen abundance (O/H) of the narrow-line regions (NLRs) of Seyfert 2 AGNs obtained through strong-line methods and from direct measurements of the electron temperature (T-e-method). The aim of this study is to explore the effects of the use of distinct methods on the range of metallicity and on the mass-metallicity relation of active galactic nuclei (AGNs) at low redshifts (z less than or similar to 0.4). We used the Sloan Digital Sky Survey (SDSS) and NASA/IPAC Extragalactic Database (NED) to selected optical (3000 < lambda (angstrom) < 7000) emission line intensities of 463 confirmed Seyfert 2 AGNs. The oxygen abundances of the NLRs were estimated using the theoretical Storchi-Bergmann et al. calibrations, the semi-empirical N2O2 calibration, the Bayesian H II-CHI-MISTRY code and the T-e-method. We found that the oxygen abundance estimations via the strong-line methods differ from each other up to similar to 0.8 dex, with the largest discrepancies in the low-metallicity regime (12 + log(O/H) less than or similar to 8.5). We confirmed that the T-e-method underestimates the oxygen abundance in NLRs, producing unreal subsolar values. We did not find any correlation between the stellar mass of the host galaxies and the metallicity of their AGNs. This result is independent of the method used to estimate Z. (AU)

FAPESP's process: 09/54006-4 - A computer cluster for the Astronomy Department of the University of São Paulo Institute of Astronomy, Geophysics and Atmospheric Sciences and for the Cruzeiro do Sul University Astrophysics Center
Grantee:Elisabete Maria de Gouveia Dal Pino
Support type: Multi-user Equipment Program