Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates
Autor(a) principal: | |
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Data de Publicação: | 2022 |
Outros Autores: | , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/247681 |
Resumo: | For the first time, the helium abundance relative to hydrogen (He/H), which relied on direct measurements of the electron temperature, has been derived in the narrow line regions (NLRs) from a local sample of Seyfert 2 nuclei. In view of this, optical emission line intensities [3000 < λ(Å) < 7000] of 65 local Seyfert 2 nuclei (z < 0.2), taken from Sloan Digital Sky Survey Data Release 15 and additional compilation from the literature, were considered. We used photoionization model grid to derive an Ionization Correction Factor (ICF) for the neutral helium. The application of this ICF indicates that the NLRs of Seyfert 2 present a neutral helium fraction of ∼50 per cent in relation to the total helium abundance. We find that Seyfert 2 nuclei present helium abundance ranging from 0.60 to 2.50 times the solar value, while ∼85 per cent of the sample present oversolar abundance values. The derived (He/H)–(O/H) abundance relation from the Seyfert 2 is stepper than that of star-forming regions (SFs) and this difference could be due to excess of helium injected into the interstellar medium by the winds of Wolf–Rayet stars. From a regression to zero metallicity, by using Seyfert 2 estimates combined with SFs estimates, we obtained a primordial helium mass fraction Yp = 0.2441 ± 0.0037, a value in good agreement with the one inferred from the temperature fluctuations of the cosmic microwave background by the Planck Collaboration, i.e. YPlanckp=0.2471±0.0003. |
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Dors Júnior, Oli LuizValerdi, MabelFreitas-Lemes, PriscilaKrabbe, Angela CristinaRiffel, Rogemar AndréAmôres, Eduardo Brescansin deRiffel, RogérioArmah, MarkSantos, Adriano Francisco Monteiro dosOliveira Junior, Celso Benedito de2022-08-21T04:39:36Z20220035-8711http://hdl.handle.net/10183/247681001147912For the first time, the helium abundance relative to hydrogen (He/H), which relied on direct measurements of the electron temperature, has been derived in the narrow line regions (NLRs) from a local sample of Seyfert 2 nuclei. In view of this, optical emission line intensities [3000 < λ(Å) < 7000] of 65 local Seyfert 2 nuclei (z < 0.2), taken from Sloan Digital Sky Survey Data Release 15 and additional compilation from the literature, were considered. We used photoionization model grid to derive an Ionization Correction Factor (ICF) for the neutral helium. The application of this ICF indicates that the NLRs of Seyfert 2 present a neutral helium fraction of ∼50 per cent in relation to the total helium abundance. We find that Seyfert 2 nuclei present helium abundance ranging from 0.60 to 2.50 times the solar value, while ∼85 per cent of the sample present oversolar abundance values. The derived (He/H)–(O/H) abundance relation from the Seyfert 2 is stepper than that of star-forming regions (SFs) and this difference could be due to excess of helium injected into the interstellar medium by the winds of Wolf–Rayet stars. From a regression to zero metallicity, by using Seyfert 2 estimates combined with SFs estimates, we obtained a primordial helium mass fraction Yp = 0.2441 ± 0.0037, a value in good agreement with the one inferred from the temperature fluctuations of the cosmic microwave background by the Planck Collaboration, i.e. YPlanckp=0.2471±0.0003.application/pdfengMonthly notices of the royal astronomical society. Oxford. Vol. 514, no. 4 (Aug. 2022), p. 5506-5527Galáxias ativasNucleo galaticoEvolucao galaticaGalaxies : AbundancesGalaxies : ActiveGalaxies : EvolutionGalaxies : FormationGalaxies : ISMGalaxies : NucleiChemical abundances in Seyfert galaxies : IX. Helium abundance estimatesEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSTEXT001147912.pdf.txt001147912.pdf.txtExtracted Texttext/plain130128http://www.lume.ufrgs.br/bitstream/10183/247681/2/001147912.pdf.txtaccae886205c6aff2fbb18db701946e2MD52ORIGINAL001147912.pdfTexto completo (inglês)application/pdf2118339http://www.lume.ufrgs.br/bitstream/10183/247681/1/001147912.pdfca4876c266a41a5d3efa58a8815aea6bMD5110183/2476812024-05-25 06:49:06.13599oai:www.lume.ufrgs.br:10183/247681Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-05-25T09:49:06Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
title |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
spellingShingle |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates Dors Júnior, Oli Luiz Galáxias ativas Nucleo galatico Evolucao galatica Galaxies : Abundances Galaxies : Active Galaxies : Evolution Galaxies : Formation Galaxies : ISM Galaxies : Nuclei |
title_short |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
title_full |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
title_fullStr |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
title_full_unstemmed |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
title_sort |
Chemical abundances in Seyfert galaxies : IX. Helium abundance estimates |
author |
Dors Júnior, Oli Luiz |
author_facet |
Dors Júnior, Oli Luiz Valerdi, Mabel Freitas-Lemes, Priscila Krabbe, Angela Cristina Riffel, Rogemar André Amôres, Eduardo Brescansin de Riffel, Rogério Armah, Mark Santos, Adriano Francisco Monteiro dos Oliveira Junior, Celso Benedito de |
author_role |
author |
author2 |
Valerdi, Mabel Freitas-Lemes, Priscila Krabbe, Angela Cristina Riffel, Rogemar André Amôres, Eduardo Brescansin de Riffel, Rogério Armah, Mark Santos, Adriano Francisco Monteiro dos Oliveira Junior, Celso Benedito de |
author2_role |
author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Dors Júnior, Oli Luiz Valerdi, Mabel Freitas-Lemes, Priscila Krabbe, Angela Cristina Riffel, Rogemar André Amôres, Eduardo Brescansin de Riffel, Rogério Armah, Mark Santos, Adriano Francisco Monteiro dos Oliveira Junior, Celso Benedito de |
dc.subject.por.fl_str_mv |
Galáxias ativas Nucleo galatico Evolucao galatica |
topic |
Galáxias ativas Nucleo galatico Evolucao galatica Galaxies : Abundances Galaxies : Active Galaxies : Evolution Galaxies : Formation Galaxies : ISM Galaxies : Nuclei |
dc.subject.eng.fl_str_mv |
Galaxies : Abundances Galaxies : Active Galaxies : Evolution Galaxies : Formation Galaxies : ISM Galaxies : Nuclei |
description |
For the first time, the helium abundance relative to hydrogen (He/H), which relied on direct measurements of the electron temperature, has been derived in the narrow line regions (NLRs) from a local sample of Seyfert 2 nuclei. In view of this, optical emission line intensities [3000 < λ(Å) < 7000] of 65 local Seyfert 2 nuclei (z < 0.2), taken from Sloan Digital Sky Survey Data Release 15 and additional compilation from the literature, were considered. We used photoionization model grid to derive an Ionization Correction Factor (ICF) for the neutral helium. The application of this ICF indicates that the NLRs of Seyfert 2 present a neutral helium fraction of ∼50 per cent in relation to the total helium abundance. We find that Seyfert 2 nuclei present helium abundance ranging from 0.60 to 2.50 times the solar value, while ∼85 per cent of the sample present oversolar abundance values. The derived (He/H)–(O/H) abundance relation from the Seyfert 2 is stepper than that of star-forming regions (SFs) and this difference could be due to excess of helium injected into the interstellar medium by the winds of Wolf–Rayet stars. From a regression to zero metallicity, by using Seyfert 2 estimates combined with SFs estimates, we obtained a primordial helium mass fraction Yp = 0.2441 ± 0.0037, a value in good agreement with the one inferred from the temperature fluctuations of the cosmic microwave background by the Planck Collaboration, i.e. YPlanckp=0.2471±0.0003. |
publishDate |
2022 |
dc.date.accessioned.fl_str_mv |
2022-08-21T04:39:36Z |
dc.date.issued.fl_str_mv |
2022 |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
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publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/247681 |
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0035-8711 |
dc.identifier.nrb.pt_BR.fl_str_mv |
001147912 |
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http://hdl.handle.net/10183/247681 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Monthly notices of the royal astronomical society. Oxford. Vol. 514, no. 4 (Aug. 2022), p. 5506-5527 |
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info:eu-repo/semantics/openAccess |
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openAccess |
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