Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines
Autor(a) principal: | |
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Data de Publicação: | 2021 |
Outros Autores: | , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/233044 |
Resumo: | For the first time, neon abundance has been derived in the narrow line region from a sample of Seyfert 2 nuclei. In view of this, we compiled from the literature fluxes of optical and infrared (IR) narrow emission lines for 35 Seyfert 2 nuclei in the local universe (z 0.06). The relative intensities of emission lines were used to derive the ionic and total neon and oxygen abundances through electron temperature estimations (Te-method). For the neon, abundance estimates were obtained by using both Te-method and IR-method. Based on photoionization model results, we found a lower electron temperature [te(Ne iii)] for the gas phase where the Ne2 + is located in comparison with t3 for the O2 + ion. We find that the differences (D) between Ne2 +/H+ ionic abundances calculated from IR-method and Te-method (assuming t3 in the Ne2 +/H+ derivation) are similar to the derivations in star-forming regions (SFs) and they are reduced by a mean factor of ∼3 when te(Ne iii) is considered. We propose a semi-empirical Ionization Correction Factor (ICF) for the neon, based on [Ne II]12.81μm, [Ne III]15.56μm, and oxygen ionic abundance ratios. We find that the average Ne/H abundance for the Seyfert 2s sample is nearly 2 times higher than similar estimate for SFs. Finally, for the very high metallicity regime (i.e. [12 + log(O/H) 8.80]) an increase in Ne/O with O/H is found, which likely indicates secondary stellar production for the neon. |
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Armah, MarkDors Júnior, Oli LuizAydar, CatarinaCardaci, Mónica V.Hägelle, Guillermo FedericoFeltre, AnnaRiffel, RogérioRiffel, Rogemar AndréKrabbe, Angela Cristina2021-12-17T04:30:20Z20210035-8711http://hdl.handle.net/10183/233044001132827For the first time, neon abundance has been derived in the narrow line region from a sample of Seyfert 2 nuclei. In view of this, we compiled from the literature fluxes of optical and infrared (IR) narrow emission lines for 35 Seyfert 2 nuclei in the local universe (z 0.06). The relative intensities of emission lines were used to derive the ionic and total neon and oxygen abundances through electron temperature estimations (Te-method). For the neon, abundance estimates were obtained by using both Te-method and IR-method. Based on photoionization model results, we found a lower electron temperature [te(Ne iii)] for the gas phase where the Ne2 + is located in comparison with t3 for the O2 + ion. We find that the differences (D) between Ne2 +/H+ ionic abundances calculated from IR-method and Te-method (assuming t3 in the Ne2 +/H+ derivation) are similar to the derivations in star-forming regions (SFs) and they are reduced by a mean factor of ∼3 when te(Ne iii) is considered. We propose a semi-empirical Ionization Correction Factor (ICF) for the neon, based on [Ne II]12.81μm, [Ne III]15.56μm, and oxygen ionic abundance ratios. We find that the average Ne/H abundance for the Seyfert 2s sample is nearly 2 times higher than similar estimate for SFs. Finally, for the very high metallicity regime (i.e. [12 + log(O/H) 8.80]) an increase in Ne/O with O/H is found, which likely indicates secondary stellar production for the neon.application/pdfengMonthly notices of the royal astronomical society. Oxford. Vol. 508, no. 1 (Nov. 2021), p. 371-391Abundância estelarGaláxias ativasEvolucao galaticaNucleo galaticoGalaxias seyfertISM: abundancesGalaxies : abundancesGalaxies : activeGalaxies : evolutionGalaxies : nucleiGalaxies : SeyfertChemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission linesEstrangeiroinfo: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:UFRGSTEXT001132827.pdf.txt001132827.pdf.txtExtracted Texttext/plain122709http://www.lume.ufrgs.br/bitstream/10183/233044/2/001132827.pdf.txtb5e7da10ef07c4e5c74f8fe0887812e5MD52ORIGINAL001132827.pdfTexto completo (inglês)application/pdf1504368http://www.lume.ufrgs.br/bitstream/10183/233044/1/001132827.pdf20283c9f7961fd892ab24c99a8bdd62bMD5110183/2330442023-09-24 03:37:44.850542oai:www.lume.ufrgs.br:10183/233044Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-09-24T06:37:44Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
title |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
spellingShingle |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines Armah, Mark Abundância estelar Galáxias ativas Evolucao galatica Nucleo galatico Galaxias seyfert ISM: abundances Galaxies : abundances Galaxies : active Galaxies : evolution Galaxies : nuclei Galaxies : Seyfert |
title_short |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
title_full |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
title_fullStr |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
title_full_unstemmed |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
title_sort |
Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines |
author |
Armah, Mark |
author_facet |
Armah, Mark Dors Júnior, Oli Luiz Aydar, Catarina Cardaci, Mónica V. Hägelle, Guillermo Federico Feltre, Anna Riffel, Rogério Riffel, Rogemar André Krabbe, Angela Cristina |
author_role |
author |
author2 |
Dors Júnior, Oli Luiz Aydar, Catarina Cardaci, Mónica V. Hägelle, Guillermo Federico Feltre, Anna Riffel, Rogério Riffel, Rogemar André Krabbe, Angela Cristina |
author2_role |
author author author author author author author author |
dc.contributor.author.fl_str_mv |
Armah, Mark Dors Júnior, Oli Luiz Aydar, Catarina Cardaci, Mónica V. Hägelle, Guillermo Federico Feltre, Anna Riffel, Rogério Riffel, Rogemar André Krabbe, Angela Cristina |
dc.subject.por.fl_str_mv |
Abundância estelar Galáxias ativas Evolucao galatica Nucleo galatico Galaxias seyfert |
topic |
Abundância estelar Galáxias ativas Evolucao galatica Nucleo galatico Galaxias seyfert ISM: abundances Galaxies : abundances Galaxies : active Galaxies : evolution Galaxies : nuclei Galaxies : Seyfert |
dc.subject.eng.fl_str_mv |
ISM: abundances Galaxies : abundances Galaxies : active Galaxies : evolution Galaxies : nuclei Galaxies : Seyfert |
description |
For the first time, neon abundance has been derived in the narrow line region from a sample of Seyfert 2 nuclei. In view of this, we compiled from the literature fluxes of optical and infrared (IR) narrow emission lines for 35 Seyfert 2 nuclei in the local universe (z 0.06). The relative intensities of emission lines were used to derive the ionic and total neon and oxygen abundances through electron temperature estimations (Te-method). For the neon, abundance estimates were obtained by using both Te-method and IR-method. Based on photoionization model results, we found a lower electron temperature [te(Ne iii)] for the gas phase where the Ne2 + is located in comparison with t3 for the O2 + ion. We find that the differences (D) between Ne2 +/H+ ionic abundances calculated from IR-method and Te-method (assuming t3 in the Ne2 +/H+ derivation) are similar to the derivations in star-forming regions (SFs) and they are reduced by a mean factor of ∼3 when te(Ne iii) is considered. We propose a semi-empirical Ionization Correction Factor (ICF) for the neon, based on [Ne II]12.81μm, [Ne III]15.56μm, and oxygen ionic abundance ratios. We find that the average Ne/H abundance for the Seyfert 2s sample is nearly 2 times higher than similar estimate for SFs. Finally, for the very high metallicity regime (i.e. [12 + log(O/H) 8.80]) an increase in Ne/O with O/H is found, which likely indicates secondary stellar production for the neon. |
publishDate |
2021 |
dc.date.accessioned.fl_str_mv |
2021-12-17T04:30:20Z |
dc.date.issued.fl_str_mv |
2021 |
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 |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/233044 |
dc.identifier.issn.pt_BR.fl_str_mv |
0035-8711 |
dc.identifier.nrb.pt_BR.fl_str_mv |
001132827 |
identifier_str_mv |
0035-8711 001132827 |
url |
http://hdl.handle.net/10183/233044 |
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. 508, no. 1 (Nov. 2021), p. 371-391 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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