Chemical abundances in Seyfert galaxies – X. Sulphur abundance estimates

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dc.contributor.authorDors Junior, Oli Luiz
dc.contributor.authorValerdi, Mabel
dc.contributor.authorRiffel, Rogemar A.
dc.contributor.authorRiffel, Rogério
dc.contributor.authorCardaci, Mónica Viviana
dc.contributor.authorHägele, Guilhermo F.
dc.contributor.authorArmah, Mark
dc.contributor.authorRevalski, Mitchell
dc.contributor.authorFlury, Sophia
dc.contributor.authorLemes, Priscila Freitas
dc.contributor.authorAmôres, Eduardo
dc.contributor.authorKrabbe, Angela Cristina
dc.contributor.authorBinette, Luc
dc.contributor.authorFeltre, Anna
dc.contributor.authorBergmann, Thaisa Storchi
dc.date.accessioned2025-02-12T18:37:55Z
dc.date.available2025-02-12T18:37:55Z
dc.date.issued22023
dc.description.abstractFor the first time, the sulphur abundance relative to hydrogen (S/H) in the narrow-line regions of a sample of Seyfert 2 nuclei (Sy 2s) has been derived via direct estimation of the electron temperature. Narrow emission-line intensities from the Sloan Digital Sky Survey (SDSS) Data Release 17 (DR17) [in the wavelength range 3000 < λ(Å) < 9100] and from the literature for a sample of 45 nearby (z < 0.08) Sy 2s were considered. Our direct estimates indicate that Sy 2s have similar temperatures in the gas region where most of the S+ ions are located in comparison with that of star-forming regions (SFs). However, Sy 2s present higher temperature values (∼10 000 K) in the region where most of the S2+ ions are located relative to that of SFs. We derive the total sulphur abundance in the range of 6.2 􏰀 12 + log(S/H) 􏰀 7.5, corresponding to 0.1–1.8 times the solar value. These sulphur abundance values are lower by ∼0.4 dex than those derived in SFs with similar metallicity, indicating a distinct chemical enrichment of the interstellar medium (ISM) for these object classes. The sulphur abundance relative to oxygen (S/O) values for our Sy 2 sample present an abrupt (∼0.5 dex) decrease with increasing oxygen abundance relative to hydrogen (O/H) for the high-metallicity regime [12 + log(O/H) 􏰁 8.7)], what is not seen for the SFs. However, when our Sy 2 estimates are combined with those from a large sample of SFs, we did not find any dependence between S/O and O/H.
dc.description.physical19 p.
dc.description.sponsorshipCoordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
dc.description.sponsorshipFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.description.sponsorshipConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.description.uriFAPESP (2020/16416-50
dc.format.mimetypePDF
dc.identifier.affiliationUniversidade do Vale do Paraíba
dc.identifier.affiliationInstituto Nacional de Astrofísica, Optica y Electrónica
dc.identifier.affiliationUniversidade Federal de Santa Maria
dc.identifier.affiliationUniversidade Federal do Rio Grande do Sul
dc.identifier.affiliationUniversidad Nacional de La Plata
dc.identifier.affiliationSpace Telescope Science Institute
dc.identifier.affiliationUniversity of Massachusetts Amherst
dc.identifier.affiliationUniversidade Estadual de Feira de Santana
dc.identifier.affiliationUniversidad Nacional Autónoma de México
dc.identifier.affiliationUniversité Laval
dc.identifier.affiliationOsservatorio di Astrofisica e Scienza dello Spazio di Bologna
dc.identifier.bibliographicCitationDORS JUNIOR, Oli Luiz et al. Chemical abundances in Seyfert galaxies – X. Sulphur abundance estimates. Monthly Notices of the Royal Astronomical Society, v. 521, n. 2, p. 1969-1987, 2023. Disponível em: https://academic.oup.com/mnras/article/521/2/1969/7068106.
dc.identifier.doi10.1093/mnras/stad635
dc.identifier.urihttps://repositorio.univap.br/handle/123456789/570
dc.language.isoen_US
dc.publisherRoyal Astronomical Society
dc.rights.holderOli Luiz Dors Junior
dc.rights.holderMabel Valerdi
dc.subject.keywordGalaxies
dc.subject.keywordEvolution – galaxies
dc.subject.keywordActive – galaxies
dc.subject.keywordSeyfert
dc.titleChemical abundances in Seyfert galaxies – X. Sulphur abundance estimates
dc.typeArtigos de Periódicos

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