Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation
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/10183/235103 |
Resumo: | The near-infrared spectra of active galactic nuclei (AGN) present emission lines of different atomic and molecular species. The mechanisms involved in the origin of these emission lines in AGN are still not fully understood. We use J- and K-band integral field spectra of six luminous (43.1 < logLbol/(erg s−1) < 44.4) Seyfert galaxies (NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC 5506, and NGC 5899) in the local Universe (0.0039 <z< 0.0136) to investigate the gas excitation within the inner 100–300 pc radius of the galaxies at spatial resolutions of a few tens of parsecs. In all galaxies, the H2 emission originates from thermal processes with excitation temperatures in the range 2400–5200 K. In the high-line ratio (HLR) region of the H2/Brγ versus [Fe II]/Paβ diagnostic diagram, which includes 29 per cent of the spaxels, shocks are the main excitation mechanism, as indicated by the correlation between the line widths and line ratios. In the AGN region of the diagram (64 per cent of the spaxels) the H2 emission is due to the AGN radiation. The [Fe II] emission is produced by a combination of photoionization by the AGN radiation and shocks in five galaxies and is dominated by photoionization in NGC 788. The [S IX]1.2523 μm coronal emission line is present in all galaxies, and its flux distributions are extended from 80 to 185 pc from the galaxy nuclei, except for NGC 5899, in which this line is detected only in the integrated spectrum. |
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Riffel, Rogemar AndréBianchin, MarinaRiffel, RogérioStorchi-Bergmann, ThaisaSchönell Júnior, Astor JoãoHahn, Luis Gabriel DahmerDametto, Natacha ZanonDiniz, Marlon Rodrigo2022-02-12T04:53:16Z20210035-8711http://hdl.handle.net/10183/235103001129609The near-infrared spectra of active galactic nuclei (AGN) present emission lines of different atomic and molecular species. The mechanisms involved in the origin of these emission lines in AGN are still not fully understood. We use J- and K-band integral field spectra of six luminous (43.1 < logLbol/(erg s−1) < 44.4) Seyfert galaxies (NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC 5506, and NGC 5899) in the local Universe (0.0039 <z< 0.0136) to investigate the gas excitation within the inner 100–300 pc radius of the galaxies at spatial resolutions of a few tens of parsecs. In all galaxies, the H2 emission originates from thermal processes with excitation temperatures in the range 2400–5200 K. In the high-line ratio (HLR) region of the H2/Brγ versus [Fe II]/Paβ diagnostic diagram, which includes 29 per cent of the spaxels, shocks are the main excitation mechanism, as indicated by the correlation between the line widths and line ratios. In the AGN region of the diagram (64 per cent of the spaxels) the H2 emission is due to the AGN radiation. The [Fe II] emission is produced by a combination of photoionization by the AGN radiation and shocks in five galaxies and is dominated by photoionization in NGC 788. The [S IX]1.2523 μm coronal emission line is present in all galaxies, and its flux distributions are extended from 80 to 185 pc from the galaxy nuclei, except for NGC 5899, in which this line is detected only in the integrated spectrum.application/pdfengMonthly notices of the royal astronomical society. Oxford. Vol. 503, no. 4 (June 2021), p. 5161-5178Galáxias ativasNucleo galaticoGalaxias seyfertGalaxies: ActiveGalaxies: ISMGalaxies: NucleiGalaxies: SeyfertGemini NIFS survey of feeding and feedback in nearby active galaxies : IV. ExcitationEstrangeiroinfo: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:UFRGSTEXT001129609.pdf.txt001129609.pdf.txtExtracted Texttext/plain84337http://www.lume.ufrgs.br/bitstream/10183/235103/2/001129609.pdf.txtd04382054c19ab57cee3ef6d78417efcMD52ORIGINAL001129609.pdfTexto completo (inglês)application/pdf8741963http://www.lume.ufrgs.br/bitstream/10183/235103/1/001129609.pdfd04e425c36bef53c805f40905b0b8130MD5110183/2351032023-09-24 03:39:34.900971oai:www.lume.ufrgs.br:10183/235103Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-09-24T06:39:34Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
title |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
spellingShingle |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation Riffel, Rogemar André Galáxias ativas Nucleo galatico Galaxias seyfert Galaxies: Active Galaxies: ISM Galaxies: Nuclei Galaxies: Seyfert |
title_short |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
title_full |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
title_fullStr |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
title_full_unstemmed |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
title_sort |
Gemini NIFS survey of feeding and feedback in nearby active galaxies : IV. Excitation |
author |
Riffel, Rogemar André |
author_facet |
Riffel, Rogemar André Bianchin, Marina Riffel, Rogério Storchi-Bergmann, Thaisa Schönell Júnior, Astor João Hahn, Luis Gabriel Dahmer Dametto, Natacha Zanon Diniz, Marlon Rodrigo |
author_role |
author |
author2 |
Bianchin, Marina Riffel, Rogério Storchi-Bergmann, Thaisa Schönell Júnior, Astor João Hahn, Luis Gabriel Dahmer Dametto, Natacha Zanon Diniz, Marlon Rodrigo |
author2_role |
author author author author author author author |
dc.contributor.author.fl_str_mv |
Riffel, Rogemar André Bianchin, Marina Riffel, Rogério Storchi-Bergmann, Thaisa Schönell Júnior, Astor João Hahn, Luis Gabriel Dahmer Dametto, Natacha Zanon Diniz, Marlon Rodrigo |
dc.subject.por.fl_str_mv |
Galáxias ativas Nucleo galatico Galaxias seyfert |
topic |
Galáxias ativas Nucleo galatico Galaxias seyfert Galaxies: Active Galaxies: ISM Galaxies: Nuclei Galaxies: Seyfert |
dc.subject.eng.fl_str_mv |
Galaxies: Active Galaxies: ISM Galaxies: Nuclei Galaxies: Seyfert |
description |
The near-infrared spectra of active galactic nuclei (AGN) present emission lines of different atomic and molecular species. The mechanisms involved in the origin of these emission lines in AGN are still not fully understood. We use J- and K-band integral field spectra of six luminous (43.1 < logLbol/(erg s−1) < 44.4) Seyfert galaxies (NGC 788, Mrk 607, NGC 3227, NGC 3516, NGC 5506, and NGC 5899) in the local Universe (0.0039 <z< 0.0136) to investigate the gas excitation within the inner 100–300 pc radius of the galaxies at spatial resolutions of a few tens of parsecs. In all galaxies, the H2 emission originates from thermal processes with excitation temperatures in the range 2400–5200 K. In the high-line ratio (HLR) region of the H2/Brγ versus [Fe II]/Paβ diagnostic diagram, which includes 29 per cent of the spaxels, shocks are the main excitation mechanism, as indicated by the correlation between the line widths and line ratios. In the AGN region of the diagram (64 per cent of the spaxels) the H2 emission is due to the AGN radiation. The [Fe II] emission is produced by a combination of photoionization by the AGN radiation and shocks in five galaxies and is dominated by photoionization in NGC 788. The [S IX]1.2523 μm coronal emission line is present in all galaxies, and its flux distributions are extended from 80 to 185 pc from the galaxy nuclei, except for NGC 5899, in which this line is detected only in the integrated spectrum. |
publishDate |
2021 |
dc.date.issued.fl_str_mv |
2021 |
dc.date.accessioned.fl_str_mv |
2022-02-12T04:53:16Z |
dc.type.driver.fl_str_mv |
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http://hdl.handle.net/10183/235103 |
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0035-8711 |
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001129609 |
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http://hdl.handle.net/10183/235103 |
dc.language.iso.fl_str_mv |
eng |
language |
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dc.relation.ispartof.pt_BR.fl_str_mv |
Monthly notices of the royal astronomical society. Oxford. Vol. 503, no. 4 (June 2021), p. 5161-5178 |
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