Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás
Ano de defesa: | 2018 |
---|---|
Autor(a) principal: | |
Orientador(a): | |
Banca de defesa: | , |
Tipo de documento: | Dissertação |
Tipo de acesso: | Acesso aberto |
Idioma: | por |
Instituição de defesa: |
Universidade Federal de Santa Maria
Centro de Ciências Naturais e Exatas |
Programa de Pós-Graduação: |
Programa de Pós-Graduação em Física
|
Departamento: |
Física
|
País: |
Brasil
|
Palavras-chave em Português: | |
Palavras-chave em Inglês: | |
Área do conhecimento CNPq: | |
Link de acesso: | http://repositorio.ufsm.br/handle/1/15557 |
Resumo: | Active galaxies exhibit a great luminosity in central region that can not be explained only by the emission of the stars of the galaxy, but by the presence of an active galactic nucleus (AGN). In this scenario, gravitational potential energy is transformed into light energy during accretion of matter by a supermassive black hole on the so-called accretion disk, which is surrounded by a torus of gas and dust. The gas outflows are generated by the accretion disk and can be observed in the narrow-line region. Outflows can have an important impact on the host galaxy of the active nucleus. In this work, we have analyzed the impact of AGN feedback on the gas kinematics of a sample of 62 active galaxies. For this we have compared the kinematics of the active galaxy with two inactive galaxies that present the same characteristics of the host galaxy of the active nucleus, in other words, the same stellar mass, redshift, morphology and inclination. The sample of inactive galaxies (controls) have 109 galaxies. The objects of our sample were observed with integral field spectroscopy by the 2.5 meter Sloan telescope within the MaNGA survey that is part of SDSS-IV. We have performed the fitting of the galaxies observed spectra using the Gas AND Absorption Line Fitting routine, and have obtained the stellar and gas velocities fields , velocity dispersion and gas emission. Through the velocity fields we have determined the kinematic position angle (PA), in order to study the impact of AGN feedback on a galactic scale. We used the stellar velocity and gas dispersion to analyze the outflows on a smaller scale 2kpc. Comparing the difference between the PA orientation of the stellar velocity fields and the gas for the two samples, we found no clear difference between the distributions. On the other hand, the AGNs have greater difference in the fractional velocity dispersion sf rac between the gas and the stars when compared with controls. The mean value of sf rac for AGNs and controls is < sfrac >AGN= 0:04 and < sfrac >CTR= �����0:23, respectively. Therefore, sf rac may be indicative of the presence of AGN. In addition, we found a positive correlation between the [O III]l5007 luminosity and sf rac for our sample. Our main conclusion in this work is that the outflows observed for the AGNs of our sample are not intense to interfere with the kinematics of the host galaxy on a large scale, but they have an important contribution on 2kpc scale. |
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2019-02-05T13:47:14Z2019-02-05T13:47:14Z2018-07-25http://repositorio.ufsm.br/handle/1/15557Active galaxies exhibit a great luminosity in central region that can not be explained only by the emission of the stars of the galaxy, but by the presence of an active galactic nucleus (AGN). In this scenario, gravitational potential energy is transformed into light energy during accretion of matter by a supermassive black hole on the so-called accretion disk, which is surrounded by a torus of gas and dust. The gas outflows are generated by the accretion disk and can be observed in the narrow-line region. Outflows can have an important impact on the host galaxy of the active nucleus. In this work, we have analyzed the impact of AGN feedback on the gas kinematics of a sample of 62 active galaxies. For this we have compared the kinematics of the active galaxy with two inactive galaxies that present the same characteristics of the host galaxy of the active nucleus, in other words, the same stellar mass, redshift, morphology and inclination. The sample of inactive galaxies (controls) have 109 galaxies. The objects of our sample were observed with integral field spectroscopy by the 2.5 meter Sloan telescope within the MaNGA survey that is part of SDSS-IV. We have performed the fitting of the galaxies observed spectra using the Gas AND Absorption Line Fitting routine, and have obtained the stellar and gas velocities fields , velocity dispersion and gas emission. Through the velocity fields we have determined the kinematic position angle (PA), in order to study the impact of AGN feedback on a galactic scale. We used the stellar velocity and gas dispersion to analyze the outflows on a smaller scale 2kpc. Comparing the difference between the PA orientation of the stellar velocity fields and the gas for the two samples, we found no clear difference between the distributions. On the other hand, the AGNs have greater difference in the fractional velocity dispersion sf rac between the gas and the stars when compared with controls. The mean value of sf rac for AGNs and controls is < sfrac >AGN= 0:04 and < sfrac >CTR= �����0:23, respectively. Therefore, sf rac may be indicative of the presence of AGN. In addition, we found a positive correlation between the [O III]l5007 luminosity and sf rac for our sample. Our main conclusion in this work is that the outflows observed for the AGNs of our sample are not intense to interfere with the kinematics of the host galaxy on a large scale, but they have an important contribution on 2kpc scale.Galáxias ativas apresentam uma grande luminosidade na região central que não pode ser explicada apenas pela emissão das estrelas da galáxia, mas sim pela presença de um núcleo ativo (AGN). Nesse cenário, a energia potencial gravitacional é transformada em energia luminosa durante a acreção de matéria por um buraco negro supermassivo, no chamado disco de acreção, que está cercado por um toroide de gás e poeira. Os outflows de gás que são gerados pelo disco de acreção podem ser observados na região de linhas estreitas. Os outflows podem ter um importante impacto na galáxia hospedeira do núcleo ativo. Neste trabalho analisamos o impacto do feedback do AGN na cinemática do gás de uma amostra de 62 galáxias ativas. Para isso comparamos a cinemática da galáxia ativa com duas galáxias inativas que apresentam as mesmas características da galáxia hospedeira do núcleo ativo, ou seja, mesma massa estelar, redshift, morfologia e inclinação. A amostra de galáxias inativas (controles) têm 109 galáxias. Os objetos da nossa amostra foram observados com espectroscopia de campo integral pelo telescópio Sloan de 2.5 metros dentro do MaNGA survey que faz parte do SDSS-IV. Realizamos o ajuste dos espectros das galáxias observadas usando a rotina Gas AND Absorption Line Fitting, obtendo dessa forma campos velocidades estelares e do gás, dispersão de velocidades e a emissão do gás. Através dos campos de velocidades determinamos o ângulo de posição (PA) cinemático, com o objetivo de estudar o impacto do feedback do AGN em uma escala galáctica. Usamos a dispersão de velocidades estelar e do gás para analisar os outflows em uma escala menor 2kpc. Ao comparar a diferença entre a orientação do PA dos campos de velocidades estelares e do gás para as duas amostras, nós não encontramos nenhuma diferença clara entre as distribuições. Por outro lado, os AGNs têm maior diferença de dispersão de velocidades fracional sf rac entre o gás e as estrelas quando comparados com os controles. Sendo que o valor médio de sf rac para AGNs e controles é < sfrac >AGN= 0:04 e < sfrac >CTR= 0:23, respectivamente. Logo, sf rac pode ser um indicativo da presença de AGN. Além disso, achamos uma correlação positiva entre a luminosidade do [O III]l5007 e sf rac para nossa amostra. A nossa principal conclusão nessa trabalho é que os outflows observados para os AGNs da nossa amostra não são intensos para interferir na cinemática da galáxia hospedeira em uma larga escala, mas apresentam uma contribuição importante em uma escala de 2kpc.Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPESporUniversidade Federal de Santa MariaCentro de Ciências Naturais e ExatasPrograma de Pós-Graduação em FísicaUFSMBrasilFísicaAttribution-NonCommercial-NoDerivatives 4.0 Internationalhttp://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessGaláxias: ativoGaláxias: cinemática e dinâmicaGaláxias: geralGalaxies: activeGalaxies: kinematics and dynamicsGalaxies: generalCNPQ::CIENCIAS EXATAS E DA TERRA::FISICAOs primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gásThe first 62 AGN observed with SDSS-IV MANGA: stellar and gas kinematicsinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/masterThesisRiffel, Rogemar Andréhttp://lattes.cnpq.br/7535636807201892Farias, Ricardo Luciano Sonegohttp://lattes.cnpq.br/5045106337913025Dors Junior, Oli Luizhttp://lattes.cnpq.br/4238829381165820http://lattes.cnpq.br/3337428272053098Ilha, Gabriele da Silva100500000006600c32f7612-cda6-434b-8a35-df1d2e93e5362d4631b5-02b8-4f30-a762-6f451423920f3ff12ffd-62c8-4e01-bffd-5e88c21377b88776e8a5-bd14-4bec-8410-67e75236f399reponame:Biblioteca Digital de Teses e Dissertações do UFSMinstname:Universidade Federal de Santa Maria (UFSM)instacron:UFSMORIGINALDIS_PPGFISICA_2018_ILHA_GABRIELE.pdfDIS_PPGFISICA_2018_ILHA_GABRIELE.pdfDissertação de Mestradoapplication/pdf9166683http://repositorio.ufsm.br/bitstream/1/15557/1/DIS_PPGFISICA_2018_ILHA_GABRIELE.pdf6d8764ef1c2780eaddfb04fa2c45a1d4MD51CC-LICENSElicense_rdflicense_rdfapplication/rdf+xml; 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dc.title.por.fl_str_mv |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
dc.title.alternative.eng.fl_str_mv |
The first 62 AGN observed with SDSS-IV MANGA: stellar and gas kinematics |
title |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
spellingShingle |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás Ilha, Gabriele da Silva Galáxias: ativo Galáxias: cinemática e dinâmica Galáxias: geral Galaxies: active Galaxies: kinematics and dynamics Galaxies: general CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
title_short |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
title_full |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
title_fullStr |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
title_full_unstemmed |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
title_sort |
Os primeiros 62 AGNS observados com o SDSS-IV MANGA: cinemática estelar e do gás |
author |
Ilha, Gabriele da Silva |
author_facet |
Ilha, Gabriele da Silva |
author_role |
author |
dc.contributor.advisor1.fl_str_mv |
Riffel, Rogemar André |
dc.contributor.advisor1Lattes.fl_str_mv |
http://lattes.cnpq.br/7535636807201892 |
dc.contributor.referee1.fl_str_mv |
Farias, Ricardo Luciano Sonego |
dc.contributor.referee1Lattes.fl_str_mv |
http://lattes.cnpq.br/5045106337913025 |
dc.contributor.referee2.fl_str_mv |
Dors Junior, Oli Luiz |
dc.contributor.referee2Lattes.fl_str_mv |
http://lattes.cnpq.br/4238829381165820 |
dc.contributor.authorLattes.fl_str_mv |
http://lattes.cnpq.br/3337428272053098 |
dc.contributor.author.fl_str_mv |
Ilha, Gabriele da Silva |
contributor_str_mv |
Riffel, Rogemar André Farias, Ricardo Luciano Sonego Dors Junior, Oli Luiz |
dc.subject.por.fl_str_mv |
Galáxias: ativo Galáxias: cinemática e dinâmica Galáxias: geral |
topic |
Galáxias: ativo Galáxias: cinemática e dinâmica Galáxias: geral Galaxies: active Galaxies: kinematics and dynamics Galaxies: general CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
dc.subject.eng.fl_str_mv |
Galaxies: active Galaxies: kinematics and dynamics Galaxies: general |
dc.subject.cnpq.fl_str_mv |
CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
description |
Active galaxies exhibit a great luminosity in central region that can not be explained only by the emission of the stars of the galaxy, but by the presence of an active galactic nucleus (AGN). In this scenario, gravitational potential energy is transformed into light energy during accretion of matter by a supermassive black hole on the so-called accretion disk, which is surrounded by a torus of gas and dust. The gas outflows are generated by the accretion disk and can be observed in the narrow-line region. Outflows can have an important impact on the host galaxy of the active nucleus. In this work, we have analyzed the impact of AGN feedback on the gas kinematics of a sample of 62 active galaxies. For this we have compared the kinematics of the active galaxy with two inactive galaxies that present the same characteristics of the host galaxy of the active nucleus, in other words, the same stellar mass, redshift, morphology and inclination. The sample of inactive galaxies (controls) have 109 galaxies. The objects of our sample were observed with integral field spectroscopy by the 2.5 meter Sloan telescope within the MaNGA survey that is part of SDSS-IV. We have performed the fitting of the galaxies observed spectra using the Gas AND Absorption Line Fitting routine, and have obtained the stellar and gas velocities fields , velocity dispersion and gas emission. Through the velocity fields we have determined the kinematic position angle (PA), in order to study the impact of AGN feedback on a galactic scale. We used the stellar velocity and gas dispersion to analyze the outflows on a smaller scale 2kpc. Comparing the difference between the PA orientation of the stellar velocity fields and the gas for the two samples, we found no clear difference between the distributions. On the other hand, the AGNs have greater difference in the fractional velocity dispersion sf rac between the gas and the stars when compared with controls. The mean value of sf rac for AGNs and controls is < sfrac >AGN= 0:04 and < sfrac >CTR= �����0:23, respectively. Therefore, sf rac may be indicative of the presence of AGN. In addition, we found a positive correlation between the [O III]l5007 luminosity and sf rac for our sample. Our main conclusion in this work is that the outflows observed for the AGNs of our sample are not intense to interfere with the kinematics of the host galaxy on a large scale, but they have an important contribution on 2kpc scale. |
publishDate |
2018 |
dc.date.issued.fl_str_mv |
2018-07-25 |
dc.date.accessioned.fl_str_mv |
2019-02-05T13:47:14Z |
dc.date.available.fl_str_mv |
2019-02-05T13:47:14Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/masterThesis |
format |
masterThesis |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://repositorio.ufsm.br/handle/1/15557 |
url |
http://repositorio.ufsm.br/handle/1/15557 |
dc.language.iso.fl_str_mv |
por |
language |
por |
dc.relation.cnpq.fl_str_mv |
100500000006 |
dc.relation.confidence.fl_str_mv |
600 |
dc.relation.authority.fl_str_mv |
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dc.rights.driver.fl_str_mv |
Attribution-NonCommercial-NoDerivatives 4.0 International http://creativecommons.org/licenses/by-nc-nd/4.0/ info:eu-repo/semantics/openAccess |
rights_invalid_str_mv |
Attribution-NonCommercial-NoDerivatives 4.0 International http://creativecommons.org/licenses/by-nc-nd/4.0/ |
eu_rights_str_mv |
openAccess |
dc.publisher.none.fl_str_mv |
Universidade Federal de Santa Maria Centro de Ciências Naturais e Exatas |
dc.publisher.program.fl_str_mv |
Programa de Pós-Graduação em Física |
dc.publisher.initials.fl_str_mv |
UFSM |
dc.publisher.country.fl_str_mv |
Brasil |
dc.publisher.department.fl_str_mv |
Física |
publisher.none.fl_str_mv |
Universidade Federal de Santa Maria Centro de Ciências Naturais e Exatas |
dc.source.none.fl_str_mv |
reponame:Biblioteca Digital de Teses e Dissertações do UFSM instname:Universidade Federal de Santa Maria (UFSM) instacron:UFSM |
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Universidade Federal de Santa Maria (UFSM) |
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UFSM |
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UFSM |
reponame_str |
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collection |
Biblioteca Digital de Teses e Dissertações do UFSM |
bitstream.url.fl_str_mv |
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