LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs
Autor(a) principal: | |
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Data de Publicação: | 2020 |
Outros Autores: | , , , , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/222871 |
Resumo: | Context. The MBH–σ⋆ relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH–σ⋆ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio. Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ⋆) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log MBH ≤ 7.75 M⊙ and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH − σ⋆ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH–σ⋆ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion. |
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Caglar, TurgayBurtscher, LeonardBrandl, BernhardBrinchmann, JarleDavies, Richard I.Hicks, Erin K. S.Koss, MichaelLin, Ming-YiMaciejewski, Witold B.Muller-Sanchez, FranciscoRiffel, Rogemar AndréRiffel, RogérioRosario, DavidSchartmann, MarcMüller, Allan SchnorrShimizu, TaroStorchi-Bergmann, ThaisaVeilleux, SylvainXivry, Gilles Orban deBennert, Vardha N.2021-06-25T04:26:15Z20200004-6361http://hdl.handle.net/10183/222871001123347Context. The MBH–σ⋆ relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH–σ⋆ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio. Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ⋆) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log MBH ≤ 7.75 M⊙ and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH − σ⋆ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH–σ⋆ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.application/pdfengAstronomy and astrophysics. Les Ulis. Vol. 634 (Fev. 2020), A114, 29 p.Galáxias ativasNucleo galaticoBuracos negrosAccretionAccretion disksBlack hole physicsGalaxies : ActiveGalaxies : BulgesGalaxies : EvolutionGalaxies : SeyfertLLAMA : the MBH–σ⋆ relation of the most luminous local AGNsEstrangeiroinfo: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:UFRGSTEXT001123347.pdf.txt001123347.pdf.txtExtracted Texttext/plain88686http://www.lume.ufrgs.br/bitstream/10183/222871/2/001123347.pdf.txtf840fcaebe18e8999839fd226a6265c8MD52ORIGINAL001123347.pdfTexto completo (inglês)application/pdf23962843http://www.lume.ufrgs.br/bitstream/10183/222871/1/001123347.pdf92b7ac7e5b647617661aa3a4488f677fMD5110183/2228712023-07-20 03:36:53.635339oai:www.lume.ufrgs.br:10183/222871Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-20T06:36:53Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
title |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
spellingShingle |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs Caglar, Turgay Galáxias ativas Nucleo galatico Buracos negros Accretion Accretion disks Black hole physics Galaxies : Active Galaxies : Bulges Galaxies : Evolution Galaxies : Seyfert |
title_short |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
title_full |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
title_fullStr |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
title_full_unstemmed |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
title_sort |
LLAMA : the MBH–σ⋆ relation of the most luminous local AGNs |
author |
Caglar, Turgay |
author_facet |
Caglar, Turgay Burtscher, Leonard Brandl, Bernhard Brinchmann, Jarle Davies, Richard I. Hicks, Erin K. S. Koss, Michael Lin, Ming-Yi Maciejewski, Witold B. Muller-Sanchez, Francisco Riffel, Rogemar André Riffel, Rogério Rosario, David Schartmann, Marc Müller, Allan Schnorr Shimizu, Taro Storchi-Bergmann, Thaisa Veilleux, Sylvain Xivry, Gilles Orban de Bennert, Vardha N. |
author_role |
author |
author2 |
Burtscher, Leonard Brandl, Bernhard Brinchmann, Jarle Davies, Richard I. Hicks, Erin K. S. Koss, Michael Lin, Ming-Yi Maciejewski, Witold B. Muller-Sanchez, Francisco Riffel, Rogemar André Riffel, Rogério Rosario, David Schartmann, Marc Müller, Allan Schnorr Shimizu, Taro Storchi-Bergmann, Thaisa Veilleux, Sylvain Xivry, Gilles Orban de Bennert, Vardha N. |
author2_role |
author author author author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Caglar, Turgay Burtscher, Leonard Brandl, Bernhard Brinchmann, Jarle Davies, Richard I. Hicks, Erin K. S. Koss, Michael Lin, Ming-Yi Maciejewski, Witold B. Muller-Sanchez, Francisco Riffel, Rogemar André Riffel, Rogério Rosario, David Schartmann, Marc Müller, Allan Schnorr Shimizu, Taro Storchi-Bergmann, Thaisa Veilleux, Sylvain Xivry, Gilles Orban de Bennert, Vardha N. |
dc.subject.por.fl_str_mv |
Galáxias ativas Nucleo galatico Buracos negros |
topic |
Galáxias ativas Nucleo galatico Buracos negros Accretion Accretion disks Black hole physics Galaxies : Active Galaxies : Bulges Galaxies : Evolution Galaxies : Seyfert |
dc.subject.eng.fl_str_mv |
Accretion Accretion disks Black hole physics Galaxies : Active Galaxies : Bulges Galaxies : Evolution Galaxies : Seyfert |
description |
Context. The MBH–σ⋆ relation is considered a result of coevolution between the host galaxies and their supermassive black holes. For elliptical bulge hosting inactive galaxies, this relation is well established, but there is still discussion concerning whether active galaxies follow the same relation. Aims. In this paper, we estimate black hole masses for a sample of 19 local luminous active galactic nuclei (AGNs; LLAMA) to test their location on the MBH–σ⋆ relation. In addition, we test how robustly we can determine the stellar velocity dispersion in the presence of an AGN continuum and AGN emission lines, and as a function of signal-to-noise ratio. Methods. Supermassive black hole masses (MBH) were derived from the broad-line-based relations for Hα, Hβ, and Paβ emission line profiles for Type 1 AGNs. We compared the bulge stellar velocity dispersion (σ⋆) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We applied an extinction correction to the observed broad-line fluxes and we corrected the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. Results. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ log MBH ≤ 7.75 M⊙ and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH − σ⋆ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. Conclusions. We find that our sample of local luminous AGNs is consistent with the MBH–σ⋆ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion. |
publishDate |
2020 |
dc.date.issued.fl_str_mv |
2020 |
dc.date.accessioned.fl_str_mv |
2021-06-25T04:26:15Z |
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/10183/222871 |
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0004-6361 |
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001123347 |
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0004-6361 001123347 |
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http://hdl.handle.net/10183/222871 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. Les Ulis. Vol. 634 (Fev. 2020), A114, 29 p. |
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info:eu-repo/semantics/openAccess |
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openAccess |
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