Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines
dc.contributor.author | Armah, Mark | pt_BR |
dc.contributor.author | Dors Júnior, Oli Luiz | pt_BR |
dc.contributor.author | Aydar, Catarina | pt_BR |
dc.contributor.author | Cardaci, Mónica V. | pt_BR |
dc.contributor.author | Hägelle, Guillermo Federico | pt_BR |
dc.contributor.author | Feltre, Anna | pt_BR |
dc.contributor.author | Riffel, Rogério | pt_BR |
dc.contributor.author | Riffel, Rogemar André | pt_BR |
dc.contributor.author | Krabbe, Angela Cristina | pt_BR |
dc.date.accessioned | 2021-12-17T04:30:20Z | pt_BR |
dc.date.issued | 2021 | pt_BR |
dc.identifier.issn | 0035-8711 | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/233044 | pt_BR |
dc.description.abstract | 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. | en |
dc.format.mimetype | application/pdf | pt_BR |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | Monthly notices of the royal astronomical society. Oxford. Vol. 508, no. 1 (Nov. 2021), p. 371-391 | pt_BR |
dc.rights | Open Access | en |
dc.subject | Abundância estelar | pt_BR |
dc.subject | ISM: abundances | en |
dc.subject | Galáxias ativas | pt_BR |
dc.subject | Galaxies : abundances | en |
dc.subject | Galaxies : active | en |
dc.subject | Evolucao galatica | pt_BR |
dc.subject | Galaxies : evolution | en |
dc.subject | Nucleo galatico | pt_BR |
dc.subject | Galaxies : nuclei | en |
dc.subject | Galaxias seyfert | pt_BR |
dc.subject | Galaxies : Seyfert | en |
dc.title | Chemical abundances in Seyfert galaxies : VII. Direct abundance determination of neon based on optical and infrared emission lines | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 001132827 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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