Análise da anisotropia orbital de populações de galáxias em aglomerados
Autor(a) principal: | |
---|---|
Data de Publicação: | 2023 |
Tipo de documento: | Dissertação |
Idioma: | por |
Título da fonte: | Biblioteca Digital de Teses e Dissertações do UFSM |
Texto Completo: | http://repositorio.ufsm.br/handle/1/30048 |
Resumo: | In this work we analyze the velocity anisotropy profiles β(r) of the star-forming (SF), transition (T), AGN, and quiescent (Q) galaxy populations belonging to gaussian clusters in order to study the impact of a galaxy’s orbital profile on the inhibition of its star formation process, as well as the triggering or cessation of nuclear activity. Furthermore, we separately analyze the samples of galaxies in gaussian (G) and non-gaussian (NG) clusters to compare their evolutionary stages. For this investigation, we use a sample composed of 177 G clusters and 34 NG clusters, which contain 11195 and 7055 galaxies, respectively. Galaxies belonging to G clusters are classified based on the main mechanism responsible for gas ionization using BPT and WHAN diagnostic diagrams. After normalizing the radial positions and peculiar velocities of the galaxies, we group them into two "pseudo-clusters" called cluster ensembles, separating galaxies belonging to G and NG clusters. The velocity anisotropy profiles were obtained using the MAMPOSSt code and the inversion of the Jeans equations. Our results show that Q galaxies have the smallest projected distances and velocity dispersions, while SF galaxies have the highest values of radial distance and velocity dispersions. T and AGN populations exhibit similar velocity dispersions, although the AGN population is less scattered in the cluster. The profiles of ν(r), σP (R), and β(r) indicate that Q and AGN populations are close to equilibrium, whereas the T population shows some signs of non-equilibrium. The results for the SF population are consistent with an unbalanced population. We interpret these results in a scenario where a population of SF galaxies in infall, hence possessing higher kinetic energies, is affected by environmental mechanisms that transform it into a quiescent population with lower velocity dispersions. A fraction of galaxies in the process of transitioning from SF to Q may trigger nuclear activity due to environmental mechanisms, appearing as a T population with a higher degree of viralization. By separately analyzing the samples of G and NG clusters, we find that galaxies in G clusters have smaller typical distances to the cluster center as well as lower velocity dispersions compared to galaxies in NG clusters. Through the β(r) profiles, we conclude that both populations exhibit some degree of non-equilibrium, although the NG population is certainly less virialized than the G population. Finally, in the case of the G population, we argue that the signs of non-equilibrium are due to the presence of a more recently accreted population (SF). |
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2023-08-23T12:33:19Z2023-08-23T12:33:19Z2023-07-28http://repositorio.ufsm.br/handle/1/30048In this work we analyze the velocity anisotropy profiles β(r) of the star-forming (SF), transition (T), AGN, and quiescent (Q) galaxy populations belonging to gaussian clusters in order to study the impact of a galaxy’s orbital profile on the inhibition of its star formation process, as well as the triggering or cessation of nuclear activity. Furthermore, we separately analyze the samples of galaxies in gaussian (G) and non-gaussian (NG) clusters to compare their evolutionary stages. For this investigation, we use a sample composed of 177 G clusters and 34 NG clusters, which contain 11195 and 7055 galaxies, respectively. Galaxies belonging to G clusters are classified based on the main mechanism responsible for gas ionization using BPT and WHAN diagnostic diagrams. After normalizing the radial positions and peculiar velocities of the galaxies, we group them into two "pseudo-clusters" called cluster ensembles, separating galaxies belonging to G and NG clusters. The velocity anisotropy profiles were obtained using the MAMPOSSt code and the inversion of the Jeans equations. Our results show that Q galaxies have the smallest projected distances and velocity dispersions, while SF galaxies have the highest values of radial distance and velocity dispersions. T and AGN populations exhibit similar velocity dispersions, although the AGN population is less scattered in the cluster. The profiles of ν(r), σP (R), and β(r) indicate that Q and AGN populations are close to equilibrium, whereas the T population shows some signs of non-equilibrium. The results for the SF population are consistent with an unbalanced population. We interpret these results in a scenario where a population of SF galaxies in infall, hence possessing higher kinetic energies, is affected by environmental mechanisms that transform it into a quiescent population with lower velocity dispersions. A fraction of galaxies in the process of transitioning from SF to Q may trigger nuclear activity due to environmental mechanisms, appearing as a T population with a higher degree of viralization. By separately analyzing the samples of G and NG clusters, we find that galaxies in G clusters have smaller typical distances to the cluster center as well as lower velocity dispersions compared to galaxies in NG clusters. Through the β(r) profiles, we conclude that both populations exhibit some degree of non-equilibrium, although the NG population is certainly less virialized than the G population. Finally, in the case of the G population, we argue that the signs of non-equilibrium are due to the presence of a more recently accreted population (SF).Neste trabalho analisamos os perfis de anisotropia de velocidades β(r) das populações de galáxias star forming (SF), transição (T), AGN e quiescente (Q), pertencentes a aglomerados gaussianos, com o objetivo de estudar o impacto do perfil orbital de uma galáxia no processo de inibição da sua formação estelar, bem como no ativamento ou cessamento da atividade nuclear. Ademais, analisamos separadamente as amostras de galáxias de aglomerados gaussianos (G) e não gaussianos (NG), a fim de compararmos seus estágios de evolução. Para realizar essa investigação utilizamos uma amostra composta por 177 aglomerados G e 34 aglomerados NG, os quais contêm, respectivamente, 11195 e 7055 galáxias. As galáxias pertencentes a aglomerados G foram classificadas com base no principal mecanismo responsável pela ionização do gás através dos diagramas de diagnóstico BPT e WHAN. Após normalizar as posições radiais e as velocidades peculiares das galáxias, as agrupamos em dois “pseudo-aglomerados”, denominados aglomerados ensemble, separando galáxias pertencentes a aglomerados G e NG. Os perfis de anisotropia de velocidades foram obtidos utilizando-se o código MAMPOSSt e a inversão das equações de Jeans. Nossos resultados mostram que as galáxias Q são aquelas que apresentam as menores distâncias projetadas e dispersões de velocidades, enquanto as galáxias SF apresentam os maiores valores de distância radial e dispersões de velocidades. As populações T e AGN apresentam dispersões de velocidades semelhantes, embora a população AGN se encontre menos espalhada no aglomerado. Os perfis de ν(r), σP (R) e β(r) indicam que as populações Q e AGN estão próximas do equilíbrio, ao passo que a população T apresenta alguns sinais de não equilíbrio. Os resultados da população SF são compatíveis com uma população não equilibrada. Interpretamos esses resultados em um cenário no qual uma população de galáxias SF em processo de infall, portanto dotada de maiores energias cinéticas, é afetada por mecanismos ambientais que a transformam em uma população quiescente com menores dispersões de velocidades. Uma fração das galáxias no processo de transformação de SF para Q podem despertar atividade nuclear devido a mecanismos ambientais, aparecendo como uma população T com um maior grau de virialização. Ao analisarmos separadamente as amostras de aglomerados G e NG, obtemos que galáxias em aglomerados G apresentam distâncias típicas ao centro do aglomerado menores, bem como dispersões de velocidades mais baixas do que galáxias em aglomerados NG. Através dos perfis de β(r) concluímos que ambas as populações apresentam algum grau de não equilíbrio, embora a população NG certamente é menos virializada do que a população G. Por fim, no caso da população G, argumentamos que os sinais de não equilíbrio se devem à presença de uma população mais recentemente acretada (SF).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/openAccessGaláxiasAglomerados de galáxiasAnálise orbitalGalaxiesClusters of galaxiesOrbital analysisCNPQ::CIENCIAS EXATAS E DA TERRA::FISICAAnálise da anisotropia orbital de populações de galáxias em aglomeradosAnalysis of the orbital anisotropy of populations of galaxies in clustersinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/masterThesisRembold, Sandro Barbozahttp://lattes.cnpq.br/3577967628416027Trevisan, MarinaSchimoia, Jáderson da Silvahttp://lattes.cnpq.br/2776953570340826Valk, Greique Ademir100500000006600600600600600d0d79563-fe0a-4c7f-a4e2-296db53f20607ecb775a-ca6a-4d71-ab2f-6245da0dab8c2f353285-be6d-4000-a6f7-58ea92bafe1a6ffd8a84-3b30-4ae5-9d24-1510386e2d4breponame:Biblioteca Digital de Teses e Dissertações do UFSMinstname:Universidade Federal de Santa Maria (UFSM)instacron:UFSMORIGINALDIS_PPGFISICA_2023_VALK_GREIQUE.pdfDIS_PPGFISICA_2023_VALK_GREIQUE.pdfDissertaçãoapplication/pdf14090246http://repositorio.ufsm.br/bitstream/1/30048/1/DIS_PPGFISICA_2023_VALK_GREIQUE.pdfd58383281172219b02d10ce3852bd820MD51LICENSElicense.txtlicense.txttext/plain; charset=utf-81956http://repositorio.ufsm.br/bitstream/1/30048/3/license.txt2f0571ecee68693bd5cd3f17c1e075dfMD53CC-LICENSElicense_rdflicense_rdfapplication/rdf+xml; charset=utf-8805http://repositorio.ufsm.br/bitstream/1/30048/2/license_rdf4460e5956bc1d1639be9ae6146a50347MD521/300482023-08-23 09:33:19.847oai:repositorio.ufsm.br:1/30048TElDRU7Dh0EgREUgRElTVFJJQlVJw4fDg08gTsODTy1FWENMVVNJVkEKCkNvbSBhIGFwcmVzZW50YcOnw6NvIGRlc3RhIGxpY2Vuw6dhLCB2b2PDqiAobyBhdXRvciAoZXMpIG91IG8gdGl0dWxhciBkb3MgZGlyZWl0b3MgZGUgYXV0b3IpIGNvbmNlZGUgw6AgVW5pdmVyc2lkYWRlCkZlZGVyYWwgZGUgU2FudGEgTWFyaWEgKFVGU00pIG8gZGlyZWl0byBuw6NvLWV4Y2x1c2l2byBkZSByZXByb2R1emlyLCAgdHJhZHV6aXIgKGNvbmZvcm1lIGRlZmluaWRvIGFiYWl4byksIGUvb3UKZGlzdHJpYnVpciBhIHN1YSB0ZXNlIG91IGRpc3NlcnRhw6fDo28gKGluY2x1aW5kbyBvIHJlc3VtbykgcG9yIHRvZG8gbyBtdW5kbyBubyBmb3JtYXRvIGltcHJlc3NvIGUgZWxldHLDtG5pY28gZQplbSBxdWFscXVlciBtZWlvLCBpbmNsdWluZG8gb3MgZm9ybWF0b3Mgw6F1ZGlvIG91IHbDrWRlby4KClZvY8OqIGNvbmNvcmRhIHF1ZSBhIFVGU00gcG9kZSwgc2VtIGFsdGVyYXIgbyBjb250ZcO6ZG8sIHRyYW5zcG9yIGEgc3VhIHRlc2Ugb3UgZGlzc2VydGHDp8OjbwpwYXJhIHF1YWxxdWVyIG1laW8gb3UgZm9ybWF0byBwYXJhIGZpbnMgZGUgcHJlc2VydmHDp8Ojby4KClZvY8OqIHRhbWLDqW0gY29uY29yZGEgcXVlIGEgVUZTTSBwb2RlIG1hbnRlciBtYWlzIGRlIHVtYSBjw7NwaWEgYSBzdWEgdGVzZSBvdQpkaXNzZXJ0YcOnw6NvIHBhcmEgZmlucyBkZSBzZWd1cmFuw6dhLCBiYWNrLXVwIGUgcHJlc2VydmHDp8Ojby4KClZvY8OqIGRlY2xhcmEgcXVlIGEgc3VhIHRlc2Ugb3UgZGlzc2VydGHDp8OjbyDDqSBvcmlnaW5hbCBlIHF1ZSB2b2PDqiB0ZW0gbyBwb2RlciBkZSBjb25jZWRlciBvcyBkaXJlaXRvcyBjb250aWRvcwpuZXN0YSBsaWNlbsOnYS4gVm9jw6ogdGFtYsOpbSBkZWNsYXJhIHF1ZSBvIGRlcMOzc2l0byBkYSBzdWEgdGVzZSBvdSBkaXNzZXJ0YcOnw6NvIG7Do28sIHF1ZSBzZWphIGRlIHNldQpjb25oZWNpbWVudG8sIGluZnJpbmdlIGRpcmVpdG9zIGF1dG9yYWlzIGRlIG5pbmd1w6ltLgoKQ2FzbyBhIHN1YSB0ZXNlIG91IGRpc3NlcnRhw6fDo28gY29udGVuaGEgbWF0ZXJpYWwgcXVlIHZvY8OqIG7Do28gcG9zc3VpIGEgdGl0dWxhcmlkYWRlIGRvcyBkaXJlaXRvcyBhdXRvcmFpcywgdm9jw6oKZGVjbGFyYSBxdWUgb2J0ZXZlIGEgcGVybWlzc8OjbyBpcnJlc3RyaXRhIGRvIGRldGVudG9yIGRvcyBkaXJlaXRvcyBhdXRvcmFpcyBwYXJhIGNvbmNlZGVyIMOgIFVGU00Kb3MgZGlyZWl0b3MgYXByZXNlbnRhZG9zIG5lc3RhIGxpY2Vuw6dhLCBlIHF1ZSBlc3NlIG1hdGVyaWFsIGRlIHByb3ByaWVkYWRlIGRlIHRlcmNlaXJvcyBlc3TDoSBjbGFyYW1lbnRlCmlkZW50aWZpY2FkbyBlIHJlY29uaGVjaWRvIG5vIHRleHRvIG91IG5vIGNvbnRlw7pkbyBkYSB0ZXNlIG91IGRpc3NlcnRhw6fDo28gb3JhIGRlcG9zaXRhZGEuCgpDQVNPIEEgVEVTRSBPVSBESVNTRVJUQcOHw4NPIE9SQSBERVBPU0lUQURBIFRFTkhBIFNJRE8gUkVTVUxUQURPIERFIFVNIFBBVFJPQ8ONTklPIE9VCkFQT0lPIERFIFVNQSBBR8OKTkNJQSBERSBGT01FTlRPIE9VIE9VVFJPIE9SR0FOSVNNTyBRVUUgTsODTyBTRUpBIEEgVUZTTQosIFZPQ8OKIERFQ0xBUkEgUVVFIFJFU1BFSVRPVSBUT0RPUyBFIFFVQUlTUVVFUiBESVJFSVRPUyBERSBSRVZJU8ODTyBDT01PClRBTULDiU0gQVMgREVNQUlTIE9CUklHQcOHw5VFUyBFWElHSURBUyBQT1IgQ09OVFJBVE8gT1UgQUNPUkRPLgoKQSBVRlNNIHNlIGNvbXByb21ldGUgYSBpZGVudGlmaWNhciBjbGFyYW1lbnRlIG8gc2V1IG5vbWUgKHMpIG91IG8ocykgbm9tZShzKSBkbyhzKQpkZXRlbnRvcihlcykgZG9zIGRpcmVpdG9zIGF1dG9yYWlzIGRhIHRlc2Ugb3UgZGlzc2VydGHDp8OjbywgZSBuw6NvIGZhcsOhIHF1YWxxdWVyIGFsdGVyYcOnw6NvLCBhbMOpbSBkYXF1ZWxhcwpjb25jZWRpZGFzIHBvciBlc3RhIGxpY2Vuw6dhLgoKBiblioteca Digital de Teses e Dissertaçõeshttps://repositorio.ufsm.br/ONGhttps://repositorio.ufsm.br/oai/requestatendimento.sib@ufsm.br||tedebc@gmail.comopendoar:2023-08-23T12:33:19Biblioteca Digital de Teses e Dissertações do UFSM - Universidade Federal de Santa Maria (UFSM)false |
dc.title.por.fl_str_mv |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
dc.title.alternative.eng.fl_str_mv |
Analysis of the orbital anisotropy of populations of galaxies in clusters |
title |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
spellingShingle |
Análise da anisotropia orbital de populações de galáxias em aglomerados Valk, Greique Ademir Galáxias Aglomerados de galáxias Análise orbital Galaxies Clusters of galaxies Orbital analysis CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
title_short |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
title_full |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
title_fullStr |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
title_full_unstemmed |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
title_sort |
Análise da anisotropia orbital de populações de galáxias em aglomerados |
author |
Valk, Greique Ademir |
author_facet |
Valk, Greique Ademir |
author_role |
author |
dc.contributor.advisor1.fl_str_mv |
Rembold, Sandro Barboza |
dc.contributor.advisor1Lattes.fl_str_mv |
http://lattes.cnpq.br/3577967628416027 |
dc.contributor.referee1.fl_str_mv |
Trevisan, Marina |
dc.contributor.referee2.fl_str_mv |
Schimoia, Jáderson da Silva |
dc.contributor.authorLattes.fl_str_mv |
http://lattes.cnpq.br/2776953570340826 |
dc.contributor.author.fl_str_mv |
Valk, Greique Ademir |
contributor_str_mv |
Rembold, Sandro Barboza Trevisan, Marina Schimoia, Jáderson da Silva |
dc.subject.por.fl_str_mv |
Galáxias Aglomerados de galáxias Análise orbital |
topic |
Galáxias Aglomerados de galáxias Análise orbital Galaxies Clusters of galaxies Orbital analysis CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
dc.subject.eng.fl_str_mv |
Galaxies Clusters of galaxies Orbital analysis |
dc.subject.cnpq.fl_str_mv |
CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
description |
In this work we analyze the velocity anisotropy profiles β(r) of the star-forming (SF), transition (T), AGN, and quiescent (Q) galaxy populations belonging to gaussian clusters in order to study the impact of a galaxy’s orbital profile on the inhibition of its star formation process, as well as the triggering or cessation of nuclear activity. Furthermore, we separately analyze the samples of galaxies in gaussian (G) and non-gaussian (NG) clusters to compare their evolutionary stages. For this investigation, we use a sample composed of 177 G clusters and 34 NG clusters, which contain 11195 and 7055 galaxies, respectively. Galaxies belonging to G clusters are classified based on the main mechanism responsible for gas ionization using BPT and WHAN diagnostic diagrams. After normalizing the radial positions and peculiar velocities of the galaxies, we group them into two "pseudo-clusters" called cluster ensembles, separating galaxies belonging to G and NG clusters. The velocity anisotropy profiles were obtained using the MAMPOSSt code and the inversion of the Jeans equations. Our results show that Q galaxies have the smallest projected distances and velocity dispersions, while SF galaxies have the highest values of radial distance and velocity dispersions. T and AGN populations exhibit similar velocity dispersions, although the AGN population is less scattered in the cluster. The profiles of ν(r), σP (R), and β(r) indicate that Q and AGN populations are close to equilibrium, whereas the T population shows some signs of non-equilibrium. The results for the SF population are consistent with an unbalanced population. We interpret these results in a scenario where a population of SF galaxies in infall, hence possessing higher kinetic energies, is affected by environmental mechanisms that transform it into a quiescent population with lower velocity dispersions. A fraction of galaxies in the process of transitioning from SF to Q may trigger nuclear activity due to environmental mechanisms, appearing as a T population with a higher degree of viralization. By separately analyzing the samples of G and NG clusters, we find that galaxies in G clusters have smaller typical distances to the cluster center as well as lower velocity dispersions compared to galaxies in NG clusters. Through the β(r) profiles, we conclude that both populations exhibit some degree of non-equilibrium, although the NG population is certainly less virialized than the G population. Finally, in the case of the G population, we argue that the signs of non-equilibrium are due to the presence of a more recently accreted population (SF). |
publishDate |
2023 |
dc.date.accessioned.fl_str_mv |
2023-08-23T12:33:19Z |
dc.date.available.fl_str_mv |
2023-08-23T12:33:19Z |
dc.date.issued.fl_str_mv |
2023-07-28 |
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/1/30048 |
url |
http://repositorio.ufsm.br/handle/1/30048 |
dc.language.iso.fl_str_mv |
por |
language |
por |
dc.relation.cnpq.fl_str_mv |
100500000006 |
dc.relation.confidence.fl_str_mv |
600 600 600 600 600 |
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 |
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bitstream.url.fl_str_mv |
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