UNIVERSIDADE FEDERAL DO RIO GRANDE DO SUL INSTITUTO DE F ´ ISICA DEPARTAMENTO DE ASTRONOMIA Os primeiros 62 AGNs observados com o SDSS-IV MaNGA: Popula¸ c˜ oes Estelares Espacialmente Resolvidas ? N´ ıcolas Dullius Mallmann Disserta¸c˜ ao realizada sob orienta¸c˜ ao do Prof. Dr. Rog´ erio Riffel e apresentada ao Programa de P´ os-Gradua¸c˜ ao em F´ ısica da Universidade Federal do Rio Grande do Sul como requisito parcial para a obten¸c˜ao do t´ ıtulo de Mestre em F´ ısica. Porto Alegre, RS, Brasil Abril de 2018 ? Trabalho financiado pelo CNPq e pelo LIneA
Transcript
UNIVERSIDADE FEDERAL DO RIO GRANDE DO SULINSTITUTO DE FISICA
DEPARTAMENTO DE ASTRONOMIA
Os primeiros 62 AGNs observados
com o SDSS-IV MaNGA:
Populacoes Estelares Espacialmente Resolvidas?
Nıcolas Dullius Mallmann
Dissertacao realizada sob orientacao do
Prof. Dr. Rogerio Riffel e apresentada
ao Programa de Pos-Graduacao em Fısica
da Universidade Federal do Rio Grande do
Sul como requisito parcial para a obtencao
do tıtulo de Mestre em Fısica.
Porto Alegre, RS, Brasil
Abril de 2018
? Trabalho financiado pelo CNPq e pelo LIneA
Agradecimentos
Ao Rogerio Riffel que, alem de um otimo orientador, possui a paciencia de um
santo, o companheirismo de um irmao e o ouvido de um psicologo.
Aos meus amigos e colegas do departamento pelos encontros festivos, jogos de
volei e futsal e quaisquer momentos de descontracao, fundamentais para a minha
sanidade.
A minha famılia, em especial aos meus pais, meu irmao e minha prima (Luana
Dullius), pelo apoio e carinho que me fornecem... dos mais variados e peculiares
jeitos, sejam eles um abraco, alguns tapinhas nas costas ou ate mesmo um golpe de
jiu-jitsu enquanto cozinho.
ResumoUma das vertentes de estudo da evolucao de galaxias se concentra nos processos de
alimentacao (feeding) e de retroalimentacao (feedback) do nucleo ativo de galaxias
partıculas, possivelmente carregadas pelo campo magnetico, que, ao entrar em con-
tato com o meio interestelar, transferem sua energia e geram lobulos de emissao em
radio. Alem disso, estes objetos apresentam intensas linhas de emissao que por vezes
podem ser muito alargadas (podendo chegar a 10 000 km/s em casos extremos). Os
AGNs sao classificados de acordo com a sua luminosidade e com a presenca ou nao de
1Se considerarmos objetos de baixa luminosidade, como os LINERs (Low Ionization EmissionLine Regions), essa fracao pode chegar a 50% (Ho, 2008).
2
Introducao 3
uma componente alargada nas linhas de emissao, oriundas de transicoes permitidas.
A fase de nucleo ativo caracteriza um estagio crıtico da evolucao de galaxias.
Uma vez que o disco de acrescao e formado no entorno do SMBH, processos de
feedback comecam a acontecer, como: jatos de partıculas relativısticas emitidos da
parte interna do disco de acrescao, ventos emanando da regiao externa deste e ra-
diacao emitida pelo plasma quente do disco ou de sua coroa (Elvis, 2000, Ciotti
et al., 2010). Acredita-se que os processos de feeding (alimentacao do AGN) e fe-
edback (resposta do AGN) conectam o crescimento do SMBH com o crescimento de
suas galaxias hospedeiras (figura 1.1), e sao reivindicados como responsaveis pela
correlacao entre a massa do SMBH e a massa do bojo da galaxia (Somerville et al.,
2008, Kormendy & Ho, 2013). Em outras palavras, ha um cenario de co-evolucao,
onde o fluxo de gas (feeding) no kiloparsec central de galaxias, quando na fase ativa,
resulta no crescimento do bojo2 da galaxia em consonancia com o crescimento do
SMBH (Ferrarese & Merritt, 2000, Gebhardt et al., 2000). Desde os estudos pionei-
ros de Terlevich e seus colaboradores (Terlevich et al., 1990) sugere-se que o excesso
observado no azul e a diluicao das linhas em absorcao no espectro nuclear de AGNs
e devido as estrelas massivas jovens. Estudos posteriores utilizando espectroscopia
de fenda longa (Kauffmann et al., 2003, Cid Fernandes et al., 2004, Riffel et al.,
2009) encontraram um excesso nas contribuicoes de populacoes jovens das galaxias
ativas quando comparadas com as nao ativas. Esse resultado levou a proposicao de
um cenario evolutivo onde o fluxo de gas para a regiao nuclear da galaxia dispara a
formacao estelar na regiao circumnuclear que e, entao, seguida pela ignicao do pro-
cesso de atividade nuclear (Storchi-Bergmann et al., 2001, Hopkins, 2012). Neste
cenario o chamado feedback positivo do AGN poderia atuar como um catalisador e
induzir a formacao estelar na galaxia hospedeira, pois este aumenta a turbulencia
no meio interestelar como previsto por simulacoes (Gaibler et al., 2012, Ishibashi &
Fabian, 2012, Wagner et al., 2012, Zubovas et al., 2013, Bieri et al., 2015, Zubovas
& Bourne, 2017) e detectado em poucos objetos (Cresci et al., 2015, Maiolino et al.,
2017).
Modelos e simulacoes modernas de inflows de gas em torno da regiao nuclear
de galaxias predizem episodios de formacao estelar circumnuclear (Kormendy &
Ho, 2013, Heckman & Best, 2014, Zubovas & Bourne, 2017). Contudo, a partir de
estudos observacionais, nao ha um consenso se a alimentacao do AGN e a formacao
estelar ocorrem simultaneamente (Kawakatu & Wada, 2008), ou se essa alimentacao
acontece em uma fase posterior ao surto de formacao estelar (Cid Fernandes et al.,
2Somente bojo classico.
Introducao 4
Figura 1.1: Historico de formacao estelar (linha preta) e diferentes medidas da taxade crescimento de SMBH: Shankar et al. (2009) em vermelho, Aird et al. (2010) emverde e Delvecchio et al. (2014) em azul. Figura retirada de Madau & Dickinson(2014).
Introducao 5
2005, Davies et al., 2007, 2009) ou se essa nao esta relaciona com nenhuma formacao
estelar recente (Sarzi et al., 2007, Hicks et al., 2013). Neste contexto, e fundamental
para esse debate investigar se ha alguma associacao entre a formacao estelar e a
atividade nuclear levando em consideracao, particularmente, diferentes regimes de
luminosidade do AGN. Alguns resultados da literatura (Kauffmann et al., 2003,
Davies et al., 2007, Esquej et al., 2014, Ruschel-Dutra et al., 2017) sugerem que
estrelas jovens nas vizinhancas do AGN sao apenas encontradas em Seyferts com
LAGN & 1043 erg/s (i.e. taxas de acrescao acima de∼ 10−3M�/yr). Portanto, outros
processos de feeding menos eficientes podem ser suficientes para fornecer material ao
SMBH em taxas de acrescao menores. De fato, muitos dos resultados inconclusivos
em AGNs do Universo local podem ser atribuıdos a luminosidade como sendo um
“parametro oculto”, ja que as analises anteriores, de AGN do universo local, foram
focadas em objetos de baixa luminosidade (e.g. Davies et al., 2007).
Durante os ultimos anos um grande esforco observacional vem sendo feito para
tentar compreender essa co-evolucao atraves do estudo do historico de formacao
estelar e da cinematica estelar, ambos, espacialmente resolvidos nas dezenas de par-
secs centrais das AGNs. O nosso grupo, ate o presente momento, estudou poucas
galaxias Seyfert do universo local utilizando cubos de dados na regiao do infraver-
melho proximo. Um dos principais resultados e que existe uma correlacao espacial
entre estrelas com baixa dispersao de velocidades e populacoes estelares de idade in-
termediaria (Riffel et al., 2010, 2011, Storchi-Bergmann et al., 2012, Schonell et al.,
2017, Diniz et al., 2017). Vale ressaltar que, apesar de inumeros estudos do historico
de formacao estelar (Star Formation History ; SFH) em galaxias terem utilizado cu-
bos de dados (e.g. de Amorim et al., 2017, Goddard et al., 2017a,b, Zheng et al.,
2017, Sanchez et al., 2017,e referencias), ate onde sabemos, nao existe nenhum es-
tudo focado em AGNs explorando, por exemplo, os efeitos da luminosidade do AGN
no SFH das galaxias hospedeiras.
1.2 Motivacao e Objetivos
Um importante avanco na compreensao do AGN e seu papel na distribuicao das
populacoes estelares pode ser alcancado atraves de uma investigacao da presenca
ou nao de estrelas jovens ou de idades intermediarias nas poucas centenas de pc do
nucleo ativo. Neste contexto: (i) se estrelas jovens dominam a contribuicao lumi-
nosa, a alimentacao do AGN e a formacao estelar ocorrem concomitantemente; (ii)
se estrelas de idade intermediarias dominarem a populacao estelar, a alimentacao
Introducao 6
do AGN seria devida a massa ejetada pelas estrelas evoluıdas, assim a fase de AGN
seria posterior a fase de formacao estelar (post-starburt phase); (iii) se apenas en-
contrarmos populacoes estelares velhas o inflow de gas para o AGN e eficiente e
a formacao estelar nao ocorre. Pelo dito acima fica evidente que para o avanco na
compreensao dos processos envolvidos na alimentacao do SMBH e necessario mapear
as populacoes estelares nas regioes centrais de uma amostra de AGNs e compara-la
com uma amostra de galaxias inativas com mesmas caracterısticas.
Nosso objetivo aqui e fazer um estudo piloto e mapear espacialmente o historico
de formacao estelar em AGNs e compara-lo com o de galaxias inativas com as mesmas
propriedades das galaxias hospedeiras de AGNs (ex. luminosidade, massa estelar,
tipo de Hubble, etc), e estudar os efeitos da luminosidade do AGN na formacao
estelar. Para tal, selecionamos os primeiros 62 AGNs observados no survey Mapping
Nearby Galaxies at Apache Point Observatory (MaNGA) e criamos uma amostra
de controle composta por galaxias inativas para comparacao. O MaNGA e a selecao
da amostra sao descritos no Cap. 2.
Capıtulo 2
Os primeiros 62 AGNs do MaNGA
2.1 MaNGA
MaNGA e um dos tres principais programas do Sloan Digital Sky Survey de quarta
geracao (SDSS-IV). O projeto, liderado por Kevin Bundy (Bundy et al., 2015),
tem como objetivo investigar a estrutura cinematica e composicao quımica do gas e
estrelas e, com isso, entender a evolucao das galaxias e os processos que regulam a
formacao de suas componentes. Para tal, o MaNGA ira mapear o fluxo de ∼ 10 000
galaxias proximas (〈z〉 ≈ 0.03) com massas estelares M? > 109M� ate o final do
projeto (em 2020).
O MaNGA utiliza um telescopio de 2,5 metros do Sloan, dedicado ao SDSS, no
Apache Point Observatory (APO). As observacoes sao feitas com unidades de campo
integral (Integral Field Unit ; IFU) compostos por um conjunto de 19 a 127 fibras
opticas agrupados em estruturas hexagonais, cobrindo campos de 12′′ a 32′′. Uma
(a) (b)
Figura 2.1: Exemplo (a) de um conjunto de fibras do IFU do MaNGA, compostopor 127 fibras, e (b) do campo de observacao para a galaxia MaNGA ID 1-114306.
7
Os primeiros 62 AGNs do MaNGA 8
imagem do IFU pode ser vista na figura 2.1a e um exemplo do campo observado na
figura 2.1b. Cada fibra alimenta um dos dois espectrografos BOSS, desenvolvidos
anteriormente para o SDSS-III (Smee et al., 2013), que sao capazes de fornecer
uma cobertura espectral de 3600 A a 10300 A, com um poder de resolucao medio
de R ∼ 2000. Para uma leitura mais tecnica do design do IFU e estrategias de
observacao, recomenda-se ler Drory et al. (2015) e Law et al. (2015).
2.2 Nossa Amostra
A amostra de 62 AGNs utilizada nesse trabalho e uma subamostra das 2778 galaxias
do MaNGA Public Launch 5 (MPL-5), selecionada por Rembold et al. (2017). Da-
dos espectrais dessas galaxias, obtidas no Data Release 12 (DR12) do SDSS-III,
foram utilizados para calcular tanto fluxos de linhas quanto larguras equivalentes
(Hβ, Hα, [OIII]λ5007, [NII]λ6584). Com os valores de fluxos e larguras equivalen-
tes, a identificacao das galaxias ativas foi realizada empregando dois diagramas di-
agnostico, BPT (Baldwin et al., 1981) que envolve as razoes de linhas [NII]λ6584/Hα
× [OIII]λ5007/Hβ e WHAN (Cid Fernandes et al., 2010, 2011) que usa a razao
[NII]λ6584/Hα × EW(Hα). Esses diagramas foram desenvolvidos para identificar o
mecanismo de ionizacao do gas que produz as linhas de emissao observadas. Para
que uma galaxia observada pelo MaNGA fosse classificada como AGN e, consequen-
temente, adicionada a nossa amostra, ela deve ser classificada como AGN em ambos
os diagramas citados – ver figura 2.2. A necessidade de utilizar ambos os diagra-
mas se da pelo fato do diagrama BPT nao diferenciar AGNs com baixa ionizacao
de galaxias com linhas de emissao geradas por estrelas evoluıdas de baixa massa,
caracterizadas por EW(Hα) < 3 A (Cid Fernandes et al., 2010).
Uma segunda amostra, contendo galaxias inativas do MPL-5, foi selecionada
atraves do pareamento de propriedades fısicas dos AGNs desse trabalho. Para cons-
truir essa amostra, foram selecionadas diversas galaxias inativas, para cada AGN,
cujo redshift z e massa estelar M? nao diferissem por 30% dos respectivos valores
da galaxia ativa. Atraves da analise morfologica (razao dos eixos, tipo de Hubble,
presenca de barras, etc.), o numero de candidatas a controle foi reduzido, chegando
em alguns casos a duas galaxias por AGN. Para manter a amostra de controle mais
homogenea, foram escolhidas apenas as 2 melhores galaxias de controle para cada
galaxia ativa. A selecao resultou em uma amostra de controle com 109 objetos (ao
inves de 124) pois 12 objetos da amostra de controle foram pareados com mais de
um AGN. A figura 2.3 mostra a distribuicao das amostras desse trabalho para qua-
Os primeiros 62 AGNs do MaNGA 9
Figura 2.2: Diagramas BPT e WHAN gerados para a amostra do MPL-5 doMaNGA. Pontos cinzas sao todas as galaxias com linhas de emissao do MPL-5,pontos pretos (azuis) sao os AGNs confirmadas da amostra principal (amostra au-xiliar – galaxias nao pertencentes ao plano original de observacao do MaNGA) doMPL-5. Figura retirada de Rembold et al. (2017).
tro propriedades. Para mais detalhes da selecao das amostras, ver Rembold et al.
(2017).
Os primeiros 62 AGNs do MaNGA 10
Figura 2.3: Distribuicao das duas amostras, AGNs e galaxias de controle, paraquatro propriedades. Para o redshift, massa estelar e magnitudes na banda r asduas amostras sao semelhantes. Ja para a luminosidade L[O III], a distribuicao degalaxias ativas esta deslocada em relacao a das controles pois L[O III] e um indicadorda intensidade do AGN. Figura retirada de Rembold et al. (2017).
Capıtulo 3
O Software megacube
Um software, chamado megacube, foi desenvolvido para realizar a sıntese de po-
pulacoes estelares de mais de 150 cubos de dados, cada qual com centenas de espec-
tros. Esse software foi projetado para trabalhar com diversos cubos de dados em
paralelo, utilizando processos filhos independentes. As figuras 3.1 e 3.2 apresentam
os fluxogramas do megacube e de um processo filho, respectivamente.
O primeiro passo realizado pelo megacube e carregar um arquivo de confi-
guracao geral, responsavel pelo controle do fluxo de operacoes dos processos filhos.
Apos a leitura, o programa importa os modulos e funcoes necessarios, alem de ob-
ter a lista de cubos de dados, indicados no arquivo de configuracao. O programa,
entao, distribui as funcoes e cubos de dados para processos filhos que, por sua vez,
sao executados em paralelo (o numero de processos filhos simultaneos e indicado por
um parametro). Quando o todos os cubos de dados foram processados, o programa
termina.
Uma das preocupacoes com a criacao do megacube foi desenvolver uma fer-
ramenta que pudesse ser rapidamente adaptada para: (i) trabalhar com cubos de
dados de diferentes surveys, (ii) executar diferentes codigos de sıntese de populacoes
estelares (ou ate mesmo outras funcoes computacionais, como algoritmos para me-
didas de fluxos de linhas) e (iii) gerar diferentes resultados conforme o objetivo do
trabalho. Com isso em mente, desenvolvemos esse codigo com capacidade modular,
ou seja, pedacos do codigo sao carregados dinamicamente atraves dos parametros
do arquivo de configuracao. Alem disso, para que a comunicacao entre os diferentes
modulos possa acontecer, a passagem de parametros e feita atraves da atualizacao
do arquivo de configuracao.
Nesse trabalho, desenvolvemos tres modulos: extracao, sıntese e analise. A figura
3.2 esquematiza a execucao dos tres modulo pelos processos filhos do megacube.
Figura 3.1: Fluxograma esquematizando o programa megacube.
O Software megacube 13
Início. ProcessoFilho
Primeiro Módulo:Extração
Lê arquivo deconfiguração.
Atualizaarquivo de
configuração.
Segundo Módulo:Síntese
Terceiro Módulo:Análise
input
Atualizaarquivo de
configuração.
input
Fim.
Espectrosextraídos.
output
input
Espectrossintetizados.
output
inputAtualiza
arquivo deconfiguração.
Cubo de dados,mapas, perfis,
gradientes, etc.
Figura 3.2: Fluxograma esquematizando a sub-rotina do megacube.
O Software megacube 14
Descrevemos as funcoes dos tres modulos nas secoes 3.1, 3.2, 3.3.
3.1 Extracao de Dados
O modulo de extracao foi desenvolvido para converter os espectros dos cubos de
dados do MaNGA para um formato aceito pelo programa de sıntese de populacoes
estelares (nesse trabalho, starlight, sec. 3.2.1). Os espectros sao preparados, antes
da extracao, conforme as seguintes etapas:
• Aplicacao do filtro Butterworth bidimensional para remover dados espurios
(sem a necessidade de combinar spaxels do cubo, como no metodo Voronoi
binning). Essa filtragem permite uma exploracao dos parametros espaciais
sem grandes perdas de resolucao;
• Aplicacao da correcao por avermelhamento galatico usando o os mapas de
Schlegel (Schlegel et al., 1998) e da lei de avermelhamento CCM (Cardelli
et al., 1989);
• Correcao do deslocamento redshift usando os parametros fornecidos pelas ta-
belas de dados do MaNGA (drpall), valores do SDSS-III;
• Espectros com sinal ruıdo SNR< 10, calculados dentro dos limites 5650-
5750 A, foram excluıdos da sıntese.
Apos as correcoes, arquivos ASCII foram criados para cada spaxel contendo
quatro parametros: comprimento de onda λ, fluxo fλ, incerteza eλ e a mascara mλ
(indicando se os dados contem problemas).
3.2 Sıntese de Populacoes Estelares
A funcao principal desse modulo e executar o codigo de sıntese de populacoes estela-
res starlight (Cid Fernandes et al., 2004, 2005). Para tal, sao gerados arquivos de
configuracao necessarios para realizar a sıntese. Alem disso, esse modulo pode sub-
dividir a lista dos espectros para que mais de uma instancia do codigo starlight
possa rodar em paralelo e, assim, acelerar o processo de sıntese do cubo inteiro. Um
exemplo de espectro sintetizado pode ser visto na figura 3.3.
O Software megacube 15
Figura 3.3: Exemplo de sıntese espectral para o spaxel central da galaxia MaNGA ID1-635503. O primeiro painel mostra o espectro observado em preto e o sintetizadoem vermelho, ambos normalizados em λ0 = 5700A. O segundo painel mostra oresıduo da sıntese. Linhas em emissao nao sao ajustadas pela sıntese de populacoesestelares.
O Software megacube 16
3.2.1 O Codigo starlight
starlight e uma ferramenta de sıntese de populacoes estelares cuja funcao e buscar
o melhor espectro sintetizado a partir de um espectro observado. Para tal finalidade,
o programa utiliza um conjunto base de N? modelos – nesse trabalho, modelos de
de estrelas com mesma idade e mesma metalicidade. Sao utilizados SSPs calculadas
por Bruzual & Charlot (2003), cujos parametros variam entre 3 metalicidades (Z
= 0.002, 0.04 e 0.05) e 15 idades (10 Myr ≤ t ≤ 13 Gyr), por serem amplamente
utilizados na literatura. Uma lei de potencia do tipo Fν ∝ ν−1.5 foi utilizada em
conjunto com as SSPs para dar conta do contınuo do espectro gerado pelo nucleo
ativo. O programa trabalha com a seguinte equacao para o espectro modelo:
Mλ = Mλ0
[N?∑n=1
xj bj,λ rλ
]⊗G(v?, σ?) (3.1)
na qual Mλ0 e o fluxo sintetico no comprimento de onda normalizado em λ0, j
representa cada uma das SSPs da base utilizada, bj,λ e o espectro da SSP, rλ e
a componente de avermelhado da SSP e xj e o vetor de populacao. A soma e
convoluıda com uma distribuicao gaussiana representada por G(v?, σ?), onde v? e
a velocidade central da distribuicao e σ? e a dispersao de velocidades. Para obter
os melhores resultados, o starlight busca minimizar uma funcao que represente
o afastamento do espectro sintetizado com relacao ao observado – quanto maior o
valor, pior e a sıntese. A funcao utilizada e o χ2 :
χ2 =
λf∑λi
[(Oλ −Mλ)ωλ]2 (3.2)
onde Oλ e o espectro medido, Mλ e o espectro sintetizado, wλ e o peso correspondente
ao comprimento de onda λ (cujo valor pode ser nulo a fim de mascarar, por exemplo,
as linhas de emissao de AGNs ou dados espurios) e λ percorre todo o intervalo de
comprimentos de onda escolhido para a sıntese.
3.3 Analise dos Dados
O terceiro modulo desenvolvido para o megacube utiliza os cubos de dados esten-
didos criados pelo modulo da sıntese para gerar os seguintes resultados:
• Mapas RGB: mapa representando, de modo qualitativo, a distribuicao relativa
O Software megacube 17
de populacoes com diferentes idades. O calculo dos mapas e feito relacionando
as cores vermelha, verde e azul aos mapas de populacoes velhas, de idade
intermediaria e jovens, respectivamente;
• Perfis radiais medios: para cada mapa estudado neste trabalho, foram gerados
30 perfis radiais igualmente espacados, com um deslocamento angular maximo
de θmax = tan−1[b/a] (relativo ao semieixo maior), onde a e o comprimento do
semieixo maior e b do semieixo menor (ver figura 3.4). Optamos por nao gerar
perfis proximos ao semieixo menor devido a inclinacao da galaxia, que implica
em perfis mais distorcidos, obscurecidos e ruidosos. Calculamos, entao, os
perfis radiais medio e do desvio padrao.
• Gradientes radiais: com os perfis medios, foram calculados gradientes utili-
zando regressao linear para tres limites de distancia radial (em unidades de
raio efetivo Re; 0.0-0.5 Re, 0.5-1.0 Re e 0.0-1.0 Re)
• Figuras comparativas: para cada trio de galaxias, isto e, AGN e suas duas
galaxias controle, foram geradas figuras comparando mapas, perfis medios e
gradientes;
• Perfis agrupados em luminosidade de [O III]λ5007: para comparar os efei-
tos dos AGNs no historico de formacao estelar, agrupamos as galaxias ativas
conforme a luminosidade da linha de emissao do [OIII]λ5007, subdividindo
em cinco intervalos de log L[O III] [ergs/s]: 39-39.75, 39.75-40.25, 40.25-40.75,
40.75-41.25 e 41.25-42. Para cada grupo, geramos o perfil medio das galaxias
ativas, das respectivas galaxias de controle e das diferencas dos perfis das
AGNs e controles.
O Software megacube 18
Figura 3.4: Exemplo de perfis obtidos para a galaxia MaNGA-ID 1-211082. Adirecao do eixo maior e indicada pela linha azul tracejada. As semi-retas em verme-lho representam as direcoes dos perfis calculados para a galaxia. O angulo maximoentre o eixo maior e um perfil qualquer e de θmax ≈ 20.5 para essa galaxia.
Capıtulo 4
Artigo
Neste capıtulo apresentamos os resultados da sıntese de populacao estelar dos primei-
ros 62 AGNs e uma comparacao destes com os objetos de controle. Tais resultados
sao apresentados em formato de artigo, publicado no Monthly Notices of the Royal
Astronomical Society (MNRAS), Mallmann et al. (2018). Por questoes esteticas, op-
tamos por colocar neste capıtulo apenas as paginas do corpo do artigo. O apendice
do artigo foi colocado em anexo a essa dissertacao (apendice A).
19
MNRAS 000, 1–15 (2017) Preprint 11 June 2018 Compiled using MNRAS LATEX style file v3.0
The first 62 AGN observed with SDSS-IV MaNGA - II:resolved stellar populations
Sandro Barboza Rembold2,3, Rogemar A. Riffel2,3, Jaderson Schimoia1,2,3,
Luiz Nicolaci da Costa2, Vladimir Avila-Reese4, Sebastian F. Sanchez4,
Alice D. Machado2,3, Rafael Cirolini2,3, Gabriele S. Ilha2,3, Janaına C. do Nascimento1,21Departamento de Astronomia, Universidade Federal do Rio Grande do Sul - Av. Bento Goncalves 9500, Porto Alegre, RS, Brazil.2Laboratorio Interinstitucional de e-Astronomia, Rua General Jose Cristino, 77 Vasco da Gama, Rio de Janeiro, Brazil, 20921-4003Departamento de Fısica, Centro de Ciencias Naturais e Exatas, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil4Instituto de Astronomıa, Universidad Nacional Autonoma de Mexico, A. P. 70-264, C.P. 04510, Mexico, D.F., Mexico
Accepted XXX. Received YYY; in original form ZZZ
ABSTRACTWe present spatially resolved stellar population age maps, average radial profilesand gradients for the first 62 Active Galactic Nuclei (AGN) observed with SDSS-IV MaNGA to study the effects of the active nuclei on the star formation history ofthe host galaxies. These results, derived using the starlight code, are compared witha control sample of non-active galaxies matching the properties of the AGN hosts. Wefind that the fraction of young stellar populations (SP) in high-luminosity AGN ishigher in the inner (R ≤ 0.5 Re) regions when compared with the control sample;low-luminosity AGN, on the other hand, present very similar fractions of young starsto the control sample hosts for the entire studied range (1 Re). The fraction of in-termediate age SP of the AGN hosts increases outwards, with a clear enhancementwhen compared with the control sample. The inner region of the galaxies (AGN andcontrol galaxies) presents a dominant old SP, whose fraction decreases outwards. Wealso compare our results (differences between AGN and control galaxies) for the earlyand late-type hosts and find no significant differences. In summary, our results suggestthat the most luminous AGN seems to have been triggered by a recent supply of gasthat has also triggered recent star formation (t ≤ 40 Myrs) in the central region.
Key words: galaxies: active – galaxies: stellar content – galaxies: star formation
1 INTRODUCTION
An important galaxy evolution stage is characterized by theActive Galactic Nuclei (AGN), a phenomenon that occurswhen the galaxy’s supermassive black hole (SMBH) is ac-creting matter from its surroundings, i.e., the accretion disk.Subsequent feedback processes start to happen, comprisingradiation emitted by the hot gas in the accretion disc or byits corona, jets of relativistic particles, and winds emanatingfrom outer regions of the disk.
Current models and simulations of gas inflows on tensto hundreds of parsec (pc) scales around galaxy nuclei leadto episodes of circumnuclear star formation (Kormendy &Ho 2013; Heckman & Best 2014; Zubovas & Bourne 2017).Zubovas & Bourne (2017) suggests that there is a critical
AGN luminosity in which the feedback of the nuclear ac-tivity increases the fragmentation of the gas clouds. Abovethis luminosity threshold, the feedback is powerful enoughto remove the gas efficiently and stop fragmentation; forAGN luminosities under this threshold, however, the feed-back is not efficient to compress the gas to high densitiesand enhance fragmentation. However, there is no consensuson whether AGN fueling occurs at the same time as the starformation (Kawakatu & Wada 2008), or follows it duringa post-starburst phase (Cid Fernandes et al. 2005; Davieset al. 2007, 2009) or if it is not associated with any recentstar formation (Sarzi et al. 2007; Hicks et al. 2013).
A breakthrough in understanding the relation betweenthe AGN and the surrounding stellar population can bereached by a simple, but thorough, investigation of whetheryoung or intermediate age stars are present within few hun-dred pc of the AGN. If the youngest stellar types are present,
AGN fueling is coeval with star formation; if instead inter-mediate age stars dominate the stellar population, fuelingwould be driven by a post-starburst and, thus the AGNphase would follow the starburst phase; finding only old starswould imply that gas inflow to the AGN is not necessarilylinked to star formation.
Over the last few years, major observational effort tounderstand this co-evolution between AGN and the circum-nuclear stellar population is being made using spatially re-solved stellar population studies in large samples of galax-ies (Goddard et al. 2017; Zheng et al. 2017). These studies,however, are not focused on comparing AGN hosts with non-active galaxies. One recent effort focusing on such kind ofcomparison was made by Sanchez et al. (2017) who foundthat AGN hosts are mostly morphologically early-type orearly-spirals and that for a given morphology, AGN hostsare more massive, more compact, more centrally peaked, andrather pressure than rotationally-supported systems whencompared to the non-active galaxies. However, these studiesdid not use a selected control sample of galaxies to match thefundamental properties of the AGN sample, nor consideredthe dependence on the AGN luminosities.
This is the second paper of a series in which we aim atstudying the resolved stellar population as well as the gasemission properties of the AGN host galaxies observed withMaNGA and compare them with those of a control sampleof non-active galaxies. In Paper I (Rembold et al. 2017),we have presented the AGN sample so far observed withMaNGA (available through the MPL-5) and have defineda control sample matching the AGN host galaxies in termsof galaxy masses, morphology, distance and inclination. InPaper I we have also characterized the stellar populationproperties of the AGN hosts as compared with those of thecontrol sample for the single aperture SDSS-III spectrumthat covers the inner 3” diameter nuclear region, using spec-tral synthesis via the starlight program (Cid Fernandeset al. 2005).
Aimed at investigating the relation between the nuclearactivity and the hosts’ star formation history (SFH), in thepresent paper (Paper II), we use the MaNGA datacubes ofthe AGN and control sample defined in Paper I to obtainthe resolved SFH and stellar population properties for theseobjects. These properties were compared between the AGNhosts and inactive galaxies in different luminosity ranges.This paper is organized as follows: brief description of theMaNGA subsample chosen for this work (Section 2); themethod of stellar population synthesis as well as the baseset of simple stellar populations (Section 3); the results ofthe synthesis for the AGN and control sample (Section 4);a discussion comparing the stellar populations of AGN andcontrol galaxies (Section 5); and a conclusion in Section 6.
2 DATA
The study of spatially resolved properties in galaxies werealways undermined by the small sample size of past integralfield spectroscopy surveys, not to mention the less numer-ous AGN. To address this problem, the Mapping NearbyGalaxies at Apache Point Observatory (MaNGA) survey(Bundy et al. 2015) was developed to observe a large sampleof nearby galaxies with integral field spectroscopy.
MaNGA is part of the fourth generation Sloan Digi-tal Sky Survey (SDSS IV) along with APOGEE-2 (Majew-ski et al. 2017) and eBOSS (Dawson et al. 2016). The sur-vey aims to provide optical spectroscopy (3600 A-10400 A)of ∼ 10, 000 nearby galaxies (with 〈z〉 ≈ 0.03). The observa-tions are carried with fiber bundles of different sizes (19-127fibers) covering a field of 12′′ to 32′′ in diameter. The se-lected sample is divided into “primary” and “secondary” tar-gets, the former are observed up to 1.5 effective radius (Re)whilst the latter is observed up to 2.5 Re. For more details,see Drory et al. (2015); Law et al. (2015); Yan et al. (2015);Yan et al. (2016).
The data used in the present work is a sub-sample ofMaNGA data (Law et al. 2016, MPL-5’s Data ReductionPipeline, DRP) selected in Paper I. In short, the AGN wereselected from the MaNGA sample by crossmatching themwith SDSS-III data products, using then the BPT diagram[O iii]/Hβ vs. [N ii]/Hα (Baldwin et al. 1981) to select theAGN. In addition, we have used the WHAN diagram (CidFernandes et al. 2010; Cid Fernandes et al. 2011) to elimi-nate from the AGN sample the“LIERs”, or“fake AGN”. Theresulting AGN sample contains 62 objects. To study the re-lationship between AGN and the stellar populations of thehost, we have chosen two control galaxies to match each ofthe selected AGN hosts. The matching was done accord-ing to the morphology (using concentration and asymmetryindices), axial ratios, redshifts, galaxy inclination, and to-tal stellar masses. For more details regarding the AGN andcontrol sample selection, see Rembold et al. (2017).
3 STELLAR POPULATION SYNTHESIS
We have used stellar population synthesis technique in orderto derive the SFH of the galaxies of the AGN and controlsamples. We first briefly describe of the fitting code used.We then present a summary of the data preparation andprocessing pipeline we have developed to manage the fittingprocess.
3.1 Fitting code
To disentangle the contribution of each stellar population tothe integrated spectra of each spaxel in the datacubes weemployed the starlight code (Cid Fernandes et al. 2005).In summary, this code combines the spectra of a base set ofN? template spectra bj,λ – usually, simple stellar population(SSP) covering a range of ages and metallicities – in orderto reproduce the observed spectra Oλ. To generate the mod-eled spectra Mλ, the SSPs are normalized at an arbitraryλ0 wavelength, reddened by the term rλ = 10−0.4(Aλ−Aλ0 ),weighted by the population vector xj (which represents thefractional contribution of the jth SSP to the light at the nor-malization wavelength λ0), and convolved with a Gaussiandistribution G(v?, σ?) to account for the effects of velocityshifts in the central velocity v? and velocity dispersion σ?.The model spectrum can be expressed as:
Mλ = Mλ0
[N?∑n=1
xj bj,λ rλ
]⊗ G(v?, σ?) (1)
where Mλ0 is the synthetic flux at the wavelength λ0. To
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The first 62 AGN in MaNGA - II: resolved stellar populations 3
find the best parameters for the fit, the code searches for the
minimum of χ2 =∑λ f
λi[(Oλ−Mλ)ωλ]2, where ωλ is the inverse
of the error, using a simulated annealing plus Metropolisscheme. Further details on the code can be found in CidFernandes et al. (2005).
The base set used in the spectral synthesis is a reducednumber of the SSPs calculated by Bruzual & Charlot (2003).It comprises N? = 46 elements (45 SSPs + 1 featurelesscontinuum – FC – function of the form Fν ∝ ν−1.5 to rep-resent the AGN emission), spanning 15 ages (0.001, 0.003,0.005, 0.010, 0.025, 0.040, 0.101, 0.286, 0.640, 0.905, 1.43,2.50, 5.00, 11.00 and 13.00 Gyrs) and 3 metallicities (0.1,1 and 2.5 Z�). The addition of a power law is necessaryto account for the AGN continuum (Cid Fernandes et al.2004; Riffel et al. 2009). For the foreground extinction, weused the Cardelli et al. (1989, CCM) law, with RV = 3.1.The adopted normalization wavelength was λ0 = 5700 Aand the synthesis was performed for the spectral range from3800 A to 7000 A.
3.2 Data Management
In order to improve the management of the data which in-cludes starlight inputs and outputs, the compilation ofthe results and the analysis, we developed a software calledmegacube. This software is designed to work with threemain modules set up by a general configuration file. Themodular approach was chosen with adaptability in mind,e.g., if a module was programmed to work with MaNGAdatacubes’ extraction, we could replace it with one that ex-tracts another survey’s datacubes. The modules used in thiswork are (in order of execution):
i) Data preparation: This module is used to processand convert the MaNGA datacubes to a data format suitablefor the chosen stellar population fitting code (starlight).The main steps are as follows:
• Filtering of the spectra using a two-dimensional but-terworth filter to remove spurious data (e.g., spiked values)and increase the signal to noise ratio, without combiningadjacent spaxel, thus allowing to a better exploration of thespatial resolution. A better description of this technique canbe found in Riffel et al. (2016);• Galactic reddening correction of each spaxel using the
Schlegel extinction maps (Schlegel et al. 1998) and the CCMreddening law;• Redshift correction using the SDSS-III redshift pro-
vided in the drpall tables of the MaNGA database;• Estimation of the signal to noise ratio (SNR) in the
wavelength range 5650-5750 A for every spaxel;• Spaxels with SNR < 10 were excluded when performing
the fitting. This was done in order to have a good compro-mise between the spatial coverage and the reliability of thefitting results (see Cid Fernandes et al. 2004, for details).
ii) Spectral Fitting: This module is used to invokethe fitting code and compile its results as described below:
• Setting up all the configuration files needed for the fits;• Fitting each individual spaxel with starlight;• Derivation of mean ages and metallicities, as well as star
formation rates, from the starlight output;• Inclusion of both standard starlight output and derived
parameters to the original datacubes as additional exten-sions.
iii) Analysis: This module uses the fitting results toproduce maps and radial plots (see Section 4 for a betterdescription):
• RGB maps: Qualitative representation of the spatiallyresolved stellar population age distribution for each galaxy,where the colors (red, green, and blue) represent three mainage bins (see Sect. 4);• Comparison figures: for each trio of galaxies (AGN and
its two controls), panels showing the relevant properties(maps of stellar population properties derived from starlightand/or SDSS-III combined ugriz images);• Radial profiles and gradients: for each galaxy and prop-
erty, a mean profile (as well as its mean gradient value –calculated as a function of R, dX/dR) is calculated to usefor quantitative comparisons;• Gradients table: as result of the analysis, we have also
generated a Table showing the gradients of the profiles forthree different bins in terms of effective radius Re;• [O iii] λ5007 luminosity L[O iii]binned radial profiles:
Radial profiles of the stellar population properties where theprofiles for the AGN (and corresponding controls) are binnedin groups according to the AGN luminosity. These profilesare shown also for AGN subsamples binned according to thehost galaxy type: early and late-type.
It is worth mentioning that a similar organizer tool wasdeveloped by de Amorim et al. (2017) for the Calar AltoLegacy Integral Field Area (CALIFA) survey, which is a pi-oneer project of integral field spectroscopy legacy surveys.
4 RESULTS
The spectral synthesis gives as results, a number of outputparameters, but we are mostly interested in xj – the frac-tional contribution of each SSP to the total light at the nor-malization wavelength λ0, that gives the SFH of each spaxel,and from which we also obtain the mean age for each spaxel,representing the age of the stellar populations as a single pa-rameter. In addition, a valuable byproduct of the fitting isthe amount of extinction in the line of sight, parameterizedby the visual extinction AV. In Figs. 1 and 2 we illustrate thederived data products (maps, radial profiles and gradients)for two AGN and their respective control sample galaxies;the equivalent plots for the remaining of the sample is avail-able in the Appendix.
In order to represent the galaxies’ ages distribution witha single parameter at each spaxel, we calculated their lightweighted mean age (Cid Fernandes et al. 2005), as follows:
〈log tL〉 =∑N?
j=1 xj log(tj )∑N?j=1 xj
, (2)
where tj is the age of the template j. The distributions ofmean age are shown in the bottom row of the bottom leftpanels of Figs. 1 and 2.
As stated by Cid Fernandes et al. (2005), small differ-ences in ages of individual SSPs are washed away in real databy noise effects. We therefore rebinned the population vec-tors in six stellar population components (SPCs): xyy (1 Myr
MNRAS 000, 1–15 (2017)
4 N. D. Mallmann et al.SD
SS Im
age
1-44379 1-211082 1-135371
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.55 0.23 -0.30
0.18 -0.06 0.50
0.47 0.20 0.15
17.43 5.85 2.61
7.57 4.14 11.17
15.91 5.65 8.83
49.45 21.40 35.64
18.47 10.02 28.29
33.71 23.83 28.80
-58.84 -30.36 -38.25
-27.27 -14.84 -39.61
-46.93 -30.19 -37.76
-1.24 -0.53 -0.52
-0.58 -0.27 -0.83
-1.08 -0.52 -0.71
Re = 5.8 kpc Re = 7.1 kpc Re = 5.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure 1. Comparison between a late-type AGN and its control galaxies. Left side panels - Top set of panels: SDSS image (the MaNGA
field is indicated in magenta). Second row: composed RGB image using the binned population vectors [blue: young (XY: t≤40 Myr); green:intermediate age (XI: 40 <≤< 2.5Gyr); red: old (XO: t > 2.5Gyr)]. Bottom set of panels: From top to bottom: visual extinction (AV),
XY, XI, XO and mean age (< t >) maps. For display purposes we used tick marks separated by 5”. The solid horizontal line in the AVmaps represent 1 Re . Right side panels - Top: summary table with the mean gradient values for each property in 3 different Re ranges.Bottom: average radial profiles, up to 1 Re , for AGN (red color) and control (blue and green colors). Shaded area represents 1σ standard
deviation. For profiles smaller than 1 Re the gradients were calculated using extrapolated values.
MNRAS 000, 1–15 (2017)
The first 62 AGN in MaNGA - II: resolved stellar populations 5SD
SS Im
age
1-95092 1-210962 1-251279
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.25 0.06 -0.04
-0.11 0.23 0.20
0.13 0.13 0.20
9.34 0.02 2.26
-2.53 0.34 4.71
4.42 0.07 5.16
41.95 61.83 26.68
-2.00 22.34 22.69
17.22 46.69 34.60
-54.64 -63.42 -32.24
-0.26 -28.06 -35.09
-24.99 -48.96 -44.75
-0.87 -0.59 -0.37
-0.09 -0.90 -0.53
-0.47 -0.64 -0.65
Re = 4.2 kpc Re = 8.7 kpc Re = 4.4 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure 2. Comparison between an early-type AGN and its control galaxies. See Fig. 1 for description.
≤ t ≤ 10 Myr), xyo (10 Myr < t ≤ 40 Myr), xiy (40 Myr < t≤ 286 Myr), xii (286 Myr < t ≤ 905 Myr), xio (905 Myr < t≤ 2.5 Gyr), and xo (2.5 Gyr < t ≤ 13 Gyr).
We have also grouped the stellar population vector inthree major age bins, described as follows:
• Young Age: XY = xyy + xyo
• Intermediate Age: XI = xiy + xii + xio• Old Age: XO = xo
In order to visualize the spatial distribution of the pop-ulations’ relative contributions in a qualitative way, RGBimages of the galaxies were created by assigning the 3 col-ors (red, green, blue) to the binned population vectors: Red
MNRAS 000, 1–15 (2017)
6 N. D. Mallmann et al.
-10.75 -5.375 0.0 5.375 10.75arcsec
-10.75
-5.375
0.0
5.375
10.75
arcs
ec
1-23979b/a 0.625 max 32.0
Figure 3. Example of radial profile cuts on the normalizationflux map of a galaxy (MaNGA ID: 1-23979) with ≈ 32 degrees
of angle displacement from the major-axis (indicated with a blue
dashed line). Red line segments are the radial profile cuts usedto calculate the mean radial profile. Profiles closer to the minor
axis were excluded to reduce any effects of projection (the more
edge-on the galaxy is, the greater the projection distortion).
represents the old XO (2.5 Gyr < t ≤ 13 Gyr), green the inter-mediate age XI (40 Myr < t ≤ 2.6 Gyr), and blue the youngstellar populations XY (1 Myr ≤ t ≤ 40 Myr).
In the bottom right of Figs. 1 and 2 we show meanradial profiles, up to 1.0 Re, for each galaxy and property,derived using a nearest neighbor interpolation method togenerate continuous values between pixel transitions andto remove abrupt changes due to spatially discrete maps.We opted for 30 equally spaced radial profiles in the galaxyplane limited to angular distances from the major axis ofθmax = tan−1(b/a) degrees, where a and b are, respectively,the semi-major and semi-minor axis of the SDSS galaxy im-age, obtained from the MaNGA’s drpall table (calculatedusing Sersic profiles), as illustrated in Fig. 3. The reasonfor this choice of maximum displacement from the majoraxis was the fact that profiles closer to the minor axis, whenprojected, resulted too noisy, possibly due to obscuration ef-fects when the galaxies are too inclined relative to the line ofsight. Mean profiles were then calculated for each propertymap by averaging all these profiles.
We have also calculated the mean gradients of eachproperty (using the mean radial profiles) for 3 different re-gions: from 0.0 to 0.5 Re, 0.5 to 1.0 Re, and 0.0 to 1.0Re. Since we are comparing relatively low luminosity activegalaxies with a matched control sample of non-active galax-ies, the major differences should be detected in their nuclearregions. Thus, the division we used was decided based onqualitative observation of the average radial profiles, whichrevealed, in most galaxies, a trend of slope changes close to0.5 Re. Some values had to be extrapolated to a constantslope since the radial profiles could not reach 1.0 Re due topoor signal to noise ratio. These gradients for AV, XY, XIand XO, together with the gradients in mean age, are shownin a Table in the top right corner of Figs. 1 and 2.
4.1 AGN hosts versus control galaxies
For each one of the AGN we show the radial variation ofthe derived properties compared to the two control galaxiesin the Appendix. As an example, we have selected to showtwo typical sets of results in Figs. 1 and 2, the results for one“late-type” AGN (MaNGA ID 1-44379) and one “early-type”AGN (MaNGA ID 1-95092) and their control galaxies.
In the case of the late-type AGN of Fig. 1, it shows thatthe RGB maps are dominated by the contribution of oldpopulations in the centers for both the AGN hosts and thecontrol galaxies. Just outward of the nucleus, younger pop-ulations dominate the AGN and the control galaxy CRT2 abit further out, while the control galaxy CRT1 shows largercontribution of older age components also outside the nu-cleus. The extinction at the nucleus is stronger for the sec-ond control than the AGN while outwards they reach similarvalues that are higher than those of the first control. Regard-ing the contribution of the different stellar population agebins to the light at 5700 A, there is no difference betweenthe AGN and the controls for the youngest age bins, whilefor the intermediate age one, its contribution in the AGN islarger than in its control galaxies at all radii. There is also adifference for the old age bin XO, that is lower in the AGNthan in the control galaxies everywhere inside Re. These re-sults also reflect in the mean age < t >: the mean age of thestellar population is lower everywhere in the galaxy for theAGN than for the control galaxies. The table listing the gra-dients also show differences between the AGN and controlgalaxies: for the inner radial bin (0-0.5 Re) and for the fullradial range (0-1.0 Re), the AGN host galaxy shows steepergradients than the controls for all properties.
The early-type AGN case of Fig. 2 shows higher con-tribution of the old component in the central regions of thegalaxies for the AGN and its controls. In this case, however,the AGN’s RGB map shows a more homogeneous popula-tion throughout the galaxy, whilst the control galaxies’ RGBmaps show an older central region surrounded by a youngerpopulation outwards. The extinction for the AGN is largercompared with its control galaxies as can be seen in the AVprofiles. Although the AV maps show higher values for thecontrol galaxies, they are concentrated closer to the limitsof SNR ≤ 10, thus less reliable. The population profiles showa more constant distribution of ages for the AGN inside theR ≤ 1.0 Re, specially between 0.5 and 1.0 Re. This behavioris reflected in the low gradient values of the 0.5 − 1.0 Re bincompared to the control galaxies. The mean age < t > profileof the AGN shows a younger population over almost all ofthe 0−1.0 Re range, similar to the late-type case (Fig. 1. Thegradients table shows that the outer region (0.5−1.0 Re) hasa different behavior for the AGN compared to the controlgalaxies (which, in turn, behave similarly).
5 DISCUSSION
In order to test for a possible relation between the AGNluminosity and the star formation history, we compare thestellar population profiles derived for the AGN and controlsbuilding average profiles for each of five L([O iii]) bins. Wegrouped them in bins of log10 L[O iii]as follows: 39 to 39.75,39.75 to 40.25, 40.25 to 40.75, 40.75 to 41.25, and 41.25 to42, using the values for L[O iii]listed in Paper I.
MNRAS 000, 1–15 (2017)
The first 62 AGN in MaNGA - II: resolved stellar populations 7
Figure 4. L[O iii]binned mean radial profiles for the xyy (1 Myr ≤ t ≤ 10 Myr) and xyo (10 Myr < t ≤ 40 Myr) components combined.
Each color pertains to the same L[O iii]range for every plot. The columns represent the groups of AGN used to calculate the averageprofiles for the AGN, its control galaxies, and their differences. The groups are, from left to right: all AGN, early-type AGN, late-type
AGN. The rows, from top to bottom, show the average profiles for the AGN, the control galaxies (of the respective AGN group), and
the differences. The colored numbers to the right of every plot are the quantity of galaxies used to calculate the mean profile of the samecolor.
Figure 5. L[O iii]binned mean radial profiles for the xiy components (40 Myr < t ≤ 286 Myr). See figure 4 for the description.
.
In Figures 4 to 9 we show the mean radial profiles forthe different age bins (see § 4 as well as for the mean ages).In order to see if there are differences in these profiles forearly and late type galaxies, we show the results both forall the galaxies grouped together and also separated in earlyand late-type hosts. In the top panels we show the results for
the AGN hosts, in the middle panel for the correspondingcontrols and in the bottom panels the difference betweenAGN and controls. In each panel we show the five rangesof L[O iii]color coded and the respective number of objects(colored numbers) included in the average calculation. It isimportant to note that some of the AGN are not classified as
Figure 7. L[O iii]binned mean radial profiles for the xio components (905 Myr < t ≤ 2.5 Gyr). See figure 4 for the description.
early or late-type (because they could not be clearly classi-fied, e.g. could be the result of mergers), so the sum of earlyand late-type galaxies may not represent the total numberof objects (left column).
As can be seen in Fig. 4, the clearest difference in theprofiles occurs for the highest [O iii] luminosity AGN, thatshow higher contribution of the young age component thanthe controls along the whole galaxy 1. In addition, the be-
1 It is worth mentioning that we have inspected carefully the fits
havior seems not to depend on the type of host galaxy (earlyor late-type), at least up to 0.6Re. We note that this bin hasonly 4 galaxies, but if we look at the profiles individually, wefind the same behavior in each one of them. Comparing withthe non-active galaxies, the corresponding profiles are sim-ilar to the other luminosity bins. For the late-type sources,
for the highest luminosity AGN, where differences in the youngpopulation were detected, and no problems with the synthesis
quality were found.
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The first 62 AGN in MaNGA - II: resolved stellar populations 9
Figure 9. L[O iii]binned mean radial profiles for the mean age (〈log t 〉). See figure 4 for the description.
there is a clear shift in the slope at ∼ 0.7Re, for larger val-ues of Re it follows the other luminosity ranges. This, andthe fact that the differences have a slightly negative slope inall morphology groups, suggests that the AGN may enhancethe star formation process in the nuclear region (Re . 0.6).
A similar excess in the AGN as compared to controlsis also observed in the intermediate age bins xiy and xiishown in Figs. 5 and 6, although the excess seems to occurfarther from the center. A comparison between Figs. 4, 5and 6 suggests an age stratification with radius for the high-est luminosity sources, showing a larger fraction of younger
stars in the central region, with the intermediate age starscontributing more to the light in the outer regions. Regard-ing the old component, Fig. 7 shows that, as expected, thehigh-luminosity AGN has less contribution of this compo-nent than the controls, with differences ranging from ∼20%to 60%. A small trend can be observed also in this figure, inthe sense that a similar although smaller difference is alsoobserved for the second luminosity bin, with the third andfourth bins showing almost no difference when comparedwith the controls, while the lowest luminosity bin showing
MNRAS 000, 1–15 (2017)
10 N. D. Mallmann et al.
0
5
10
15
39.0
0 - 3
9.75
0
5
10
15
39.7
5 - 4
0.25
0
5
10
15
40.2
5 - 4
0.75
0
5
10
15
40.7
5 - 4
1.25
0.0 - 0.5 Re0.5 - 1.0 Re
0.0 - 1.0 Re
0
5
10
15
41.2
5 - 4
2.00
Figure 10. Young stellar population xy contribution for five different bins of luminosity (39-39.75, 39.75-40.25, 40.25-40.75, 40.75-41.25,
41.25-42), calculated for three different regions (0.0-0.5 Re , 0.5-1.0 Re , 0.0-1.0 Re). Each color represents a different AGN grouping: greenfor the late-type AGN, red for the early-type AGN, and blue for all the AGN sample. Solid lines correspond to the active galaxies and
dashed lines to the control galaxies.
the opposite: the controls having less contribution of the oldcomponent than the AGN.
In order to compare the galaxies using a single parame-ter we plot the radial profiles of their mean ages (see §4) inFig. 9. It is clear from this figure that the higher luminosityAGN hosts are younger than the control galaxies in the en-tire studied region (1Re). We interpret these results as due tothe fact that AGN hosts do prefer the “outside-in” scenariofor the recent star formation, while the galaxy’s global stel-lar formation history (SFH) is better described by an insideout scenario. This may reflect the idea that the active nuclei
can drive the star formation process in the circumnuclearregion.
Although the differences in the stellar population of thestrongest AGN, when compared with the controls, were ev-ident, a problem arises when trying to analyze other lumi-nosity bins: the differences between the radial profiles aretoo noisy. In order to circumvent this problem, we binnedthe profiles into three regions (0.0-0.5 Re, 0.5-1.0 Re, and 0.0-1.0 Re) and the stellar populations into XY, XI, xO. We alsoplotted the contribution of the FC using these radial bins toinspect the light contribution of the AGN continuum. Fig-
MNRAS 000, 1–15 (2017)
The first 62 AGN in MaNGA - II: resolved stellar populations 11
0255075
100
39.0
0 - 3
9.75
0255075
100
39.7
5 - 4
0.25
0255075
100
40.2
5 - 4
0.75
0255075
100
40.7
5 - 4
1.25
0.0 - 0.5 Re0.5 - 1.0 Re
0.0 - 1.0 Re
0255075
100
41.2
5 - 4
2.00
Figure 11. Intermediate age stellar population xi for different bins of luminosity, calculated for three different regions. See Fig. 10.
ures 10-14 show the results of this exercise2. What clearlyemerges from this test is that the youngest SPs are concen-trated in the inner 0.5 Re of the most luminous AGN hosts(Fig. 10) – where the FC signature is the strongest (Fig.14) – and intermediate age ones are located in regions withradius R & 0.5 Re (see Fig. 11) for all AGN luminosities. Inaddition, the contribution of these stellar population compo-nents are much larger in the AGN hosts (circles) than thatin the control galaxies (triangles) in the case of the high-est luminosity AGN. Another result shown by these plots
2 Some galaxies have limited Re coverage, meaning that thestatistics gets weaker with radial distance. We addressed this
problem by using radial intervals (0.5 Re).
is that the youngest age contributions increase outwards forlate-type galaxies (both controls and AGN – except the mostluminous AGN).
Figs. 12 and 13 show that the strongest (highest lu-minosity) AGN present, in general, younger SPs than theircontrol objects. In addition these plots do allow us to betteranalyze the other luminosity bins. For log(L[O iii] between40.75 and 41.25 (the second most luminous bin) no signif-icant differences can be seen for the younger populations,while the intermediate age contributions are higher for theAGN, being slightly more concentrated at the outer region(R & 0.5 Re). For the remaining luminosity bins a similarbehavior is observed, however, when looking to the overall
MNRAS 000, 1–15 (2017)
12 N. D. Mallmann et al.
0255075
100
39.0
0 - 3
9.75
0255075
100
39.7
5 - 4
0.25
0255075
100
40.2
5 - 4
0.75
0255075
100
40.7
5 - 4
1.25
0.0 - 0.5 Re0.5 - 1.0 Re
0.0 - 1.0 Re
0255075
100
41.2
5 - 4
2.00
Figure 12. Old stellar population xo for different bins of luminosity, calculated for three different regions. See Fig. 10.
mean values (right side of Fig. 11) it is clear that the differ-ence vanishes with luminosity decrease.
In the case of the old stellar population bin, the contri-bution of this population in the AGN hosts is lower than thatobserved in the control objects, and a decrease is observedfrom the center outwards. A significant difference betweenactive and non-active sources is seen for the two highest lu-minosity bins, specially when using the overall mean values(right side plot). We also separate the objects according totheir Hubble types (color coded) and no clear difference isobserved between early and late-type galaxies when compar-ing active and non-active hosts.
The above results reinforce literature results (Remboldet al. 2017; Kauffmann et al. 2003), in the sense that when
comparing low and high luminosity AGN, the contributionof old stellar populations decreases, while that of the youngerstellar populations increases in the latter. However, our re-sults do additionally show that this is specially enhancedin the circumnuclear regions (R ≤ 0.5 Re) indicating thatthe the inflow of material feeding the AGN is partially be-ing used to form stars. In addition, we suggest that thesenuclear starbursts could at least be partially related to apositive AGN feedback, which may be inducing star forma-tion in the host galaxy through enhancing the gas turbu-lence in the interstellar medium. Such a positive feedbackis predicted by simulations (Gaibler et al. 2012; Ishibashi &Fabian 2012; Wagner et al. 2012; Zubovas et al. 2013; Bieriet al. 2015; Zubovas & Bourne 2017) and was already de-
MNRAS 000, 1–15 (2017)
The first 62 AGN in MaNGA - II: resolved stellar populations 13
8.59.09.5
10.010.5
39.0
0 - 3
9.75
8.59.09.5
10.010.5
39.7
5 - 4
0.25
8.59.09.5
10.010.5
40.2
5 - 4
0.75
8.59.09.5
10.010.5
40.7
5 - 4
1.25
0.0 - 0.5 Re0.5 - 1.0 Re
0.0 - 1.0 Re
8.59.09.5
10.010.5
41.2
5 - 4
2.00
Figure 13. Mean age 〈log t 〉 for different bins of luminosity, calculated for three different regions. See Fig. 10.
tected in a few objects (Cresci et al. 2015; Maiolino et al.2017).
As can be seen from Figs.10 to 13 in general we ob-serve that the fraction of young and intermediate age stellarpopulations increases with the radius, while in the case ofthe old population, it decreases. These results support theprevious findings reported by Sanchez et al. (2013), Ibarra-Medel et al. (2016) and Goddard et al. (2017) favoring aninside-out scenario for the formation of galaxies. However,when considering the most luminous AGN, it no longer ap-plies, and it seems that these AGN have been triggered by arecent supply of gas that has also triggered a recent star for-mation in their central regions. Our findings are opposite tothe results of Goddard et al. (2017) in the case of early-typesources, we derive a slightly negative gradient while they de-
rived a slightly positive one for this Hubble class3. On theother hand, our findings seem to agree with those of Ibarra-Medel et al. (2016), who showed that the radial stellar massgrowth histories of early-type galaxies are on average nearlyinside-out, though with a trend much less pronounced thanthat of the late-type galaxies.
6 CONCLUSIONS
We studied the stellar content of the first 62 AGN observedwith SDSS-IV MaNGA and compared them with a matchedsample of inactive galaxies presented in Paper I. We con-structed spatially resolved stellar population age maps, cor-responding average radial profiles and gradients for thesesources using the starlight code, aimed at studying the
3 Note, however, that we are studying the inner 1 Re (they used
1.5 Re) and a smaller sample than that studied by these authors.
MNRAS 000, 1–15 (2017)
14 N. D. Mallmann et al.
0
5
10
15
39.0
0 - 3
9.75
0
5
10
15
39.7
5 - 4
0.25
0
5
10
15
40.2
5 - 4
0.75
0
5
10
15
40.7
5 - 4
1.25
0.0 - 0.5 Re0.5 - 1.0 Re
0.0 - 1.0 Re
0
5
10
15
41.2
5 - 4
2.00
Figure 14. Featureless continuum for different bins of luminosity, calculated for three different regions. See Fig. 10.
effects of the AGN on the star formation history of the hostgalaxies.
We found that the fraction of the young stellar popula-tion (t . 40 Myr) is related with the AGN luminosity. Forhigh-luminosity AGN (L[O iii] & 1041.25 ergs/s) it increasesin the inner (R ≤ 0.5Re) regions when compared with the ob-jects in the control sample. In the case of the low-luminosityAGN, both AGN and control sample hosts, present verysimilar fractions of young stars. This result indicates thatthe inflow of material, besides feeding the nuclear engine, isbeing used to form new stars, thus rejuvenating the stellarcontent of the nuclear region of the AGN hosts. In addi-tion, this very young starburst could also be enhanced bya positive AGN feedback produced by the high-luminosityAGN.
The fraction of the intermediate age, XI (40 Myr < t ≤2.6 Gyr), SP of the AGN hosts slightly increase outwards,with a clear enhancement over the entire galaxy when com-pared with the control sample. In addition, our results show
that the inner region of the galaxies are dominated by an oldSP, whose fraction decreases outwards. These results sup-port the previous findings of the CALIFA team (Sanchezet al. 2013), supporting an inside-out scenario for the galax-ies’ star formation history.
We also investigated for differences on the star forma-tion histories between the different Hubble types. No sig-nificant differences were found between early and late-typehosts galaxies.
From our results we suggest that an outside in scenariobetter describes the recent star formation in the AGN hosts,while an inside out scenario represents better the older gen-erations of stars.
ACKNOWLEDGEMENTS
We thank the anonymous referee for the useful commentsand suggestions. NDM thanks to CNPq for financial sup-
MNRAS 000, 1–15 (2017)
The first 62 AGN in MaNGA - II: resolved stellar populations 15
port. R.R. Thanks to FAPERGS and CNPq for financialsupport.
Funding for the Sloan Digital Sky Survey IV has beenprovided by the Alfred P. Sloan Foundation, the U.S. De-partment of Energy Office of Science, and the ParticipatingInstitutions. SDSS acknowledges support and resources fromthe Center for High-Performance Computing at the Univer-sity of Utah. The SDSS web site is www.sdss.org.
SDSS is managed by the Astrophysical Research Con-sortium for the Participating Institutions of the SDSS Col-laboration including the Brazilian Participation Group, theCarnegie Institution for Science, Carnegie Mellon Univer-sity, the Chilean Participation Group, the French Par-ticipation Group, Harvard-Smithsonian Center for Astro-physics, Instituto de Astrofısica de Canarias, The JohnsHopkins University, Kavli Institute for the Physics andMathematics of the Universe (IPMU) / University of Tokyo,Lawrence Berkeley National Laboratory, Leibniz Institut furAstrophysik Potsdam (AIP), Max-Planck-Institut fur As-tronomie (MPIA Heidelberg), Max-Planck-Institut fur As-trophysik (MPA Garching), Max-Planck-Institut fur Ex-traterrestrische Physik (MPE), National Astronomical Ob-servatories of China, New Mexico State University, NewYork University, University of Notre Dame, ObservatorioNacional / MCTI, The Ohio State University, Pennsylva-nia State University, Shanghai Astronomical Observatory,United Kingdom Participation Group, Universidad NacionalAutonoma de Mexico, University of Arizona, Universityof Colorado Boulder, University of Oxford, University ofPortsmouth, University of Utah, University of Virginia, Uni-versity of Washington, University of Wisconsin, VanderbiltUniversity, and Yale University.
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Apendice A: Comparacoes
AGN-Controles
Aqui, colocamos as imagens do apendice do artigo apresentado no capıtulo 4.
48
2SD
SS Im
age
1-109056 1-73005 1-43009
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.04 -0.03 0.11
0.08 -0.02 0.09
0.04 0.01 0.15
1.97 6.50 13.77
5.36 9.26 6.91
4.73 9.38 10.99
30.94 16.17 25.67
30.81 13.52 30.04
37.42 10.51 37.03
-35.41 -24.28 -38.53
-35.92 -35.52 -43.89
-42.54 -25.70 -50.52
-0.46 -0.48 -0.83
-0.66 -2.00 -1.08
-0.68 -0.97 -1.03
Re = 3.5 kpc Re = 6.4 kpc Re = 6.8 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A1. Comparison of the AGN with MaNGA ID 1-109056 and its control galaxies.
3SD
SS Im
age
1-121532 1-218427 1-177493
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.65 0.00 -0.02
-0.52 0.07 -0.12
-0.45 0.03 -0.08
-7.54 0.00 0.00
-1.52 0.00 0.11
-5.92 0.00 0.04
11.34 3.26 4.76
-33.61 10.15 23.34
-12.79 7.07 15.49
-16.48 -0.98 -5.69
21.60 -9.28 -29.39
12.01 -5.26 -17.78
0.06 -0.06 -0.03
-1.77 -0.09 -0.99
-0.29 -0.09 -0.35
Re = 15 kpc Re = 6.2 kpc Re = 7.7 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A2. Comparison of the AGN with MaNGA ID 1-121532 and its control galaxies.
4SD
SS Im
age
1-135044 1-218280 1-211063
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.53 0.31 -0.18
0.06 --- -0.01
-0.13 0.31 -0.11
1.64 35.65 6.99
12.10 --- 9.86
6.95 35.65 9.01
43.13 177.92 72.50
-2.18 --- -22.10
28.66 177.92 75.45
-47.65 -270.30 -91.47
-27.18 --- -27.92
-43.94 -270.30 -101.90
-0.64 -6.71 -1.25
-0.89 --- -1.46
-0.81 -6.71 -1.70
Re = 5.6 kpc Re = 26 kpc* Re = 11 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A3. Comparison of the AGN with MaNGA ID 1-135044 and its control galaxies. ∗The effective radius of this galaxy is too large
to fit in the panel (Re = 51′′).
5SD
SS Im
age
1-135285 1-633990 1-25688
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.36 -0.90 -0.27
-0.09 -0.16 -0.12
-0.09 -0.43 -0.19
0.32 -25.31 3.42
3.72 0.60 -1.29
2.06 -9.71 3.11
39.91 19.11 -5.63
20.44 15.70 28.41
41.96 37.39 14.95
-40.68 22.28 -2.16
-48.41 -33.20 -36.48
-55.27 -27.80 -25.98
-0.42 0.92 -0.16
-1.27 -0.98 -0.50
-0.82 -0.25 -0.46
Re = 7.8 kpc Re = 5.9 kpc Re = 4.3 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A4. Comparison of the AGN with MaNGA ID 1-135285 and its control galaxies.
6SD
SS Im
age
1-135641 1-635503 1-235398
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-1.39 -0.50 -1.33
-0.14 -0.61 0.40
-0.52 -0.67 -0.56
4.01 7.69 -8.95
8.39 -0.02 13.71
8.65 0.71 0.82
30.97 -3.61 -36.25
18.39 4.42 77.69
34.84 1.75 27.64
-37.91 -16.90 43.74
-42.75 -13.41 -92.12
-49.79 -18.18 -30.19
-0.53 -0.39 0.78
-0.69 -0.23 -1.22
-0.80 -0.33 -0.23
Re = 7.7 kpc Re = 6.2 kpc Re = 5.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.2
0.4
0.6
0.8
1.0
1.2
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A5. Comparison of the AGN with MaNGA ID 1-135641 and its control galaxies. It is important to note that the artifact
present on the galaxy 1-635503 (the ring on the maps) is just the result of the spaxels’ exclusion mask we used (MaNGA bit signalinga foreground star and S/N cutoff) and have no effect on our results. A similar situation occurs in other results, such as in Figs. A7 and
A12.
7SD
SS Im
age
1-137883 1-178838 1-36878
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-1.10 0.25 -0.79
-1.33 0.29 -0.90
-1.33 0.29 -0.77
-3.35 4.04 15.20
-12.72 2.78 -13.14
-9.54 4.66 0.90
43.63 1.86 11.73
20.04 24.26 -6.70
49.02 8.93 2.38
-40.70 -6.72 -34.33
-17.42 -30.80 24.47
-44.58 -16.16 -5.09
-0.29 -0.20 -0.82
0.37 -0.41 1.64
-0.09 -0.34 0.14
Re = 3.0 kpc Re = 1.7 kpc Re = 5.0 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.41.6
0.25
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0.75
1.00
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<t [l
og(y
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8.0
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10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A6. Comparison of the AGN with MaNGA ID 1-137883 and its control galaxies.
8SD
SS Im
age
1-148068 1-166947 1-55572
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.26 0.37 0.20
0.09 -1.04 0.17
0.08 0.39 0.36
6.72 6.71 2.76
2.90 6.15 14.67
9.57 8.06 9.14
48.86 43.99 44.77
51.67 -43.29 -5.17
59.34 37.24 54.71
-47.74 -56.70 -45.91
-60.99 -53.74 -60.90
-69.26 -61.72 -76.95
-0.84 -1.18 -0.68
-0.92 -8.50 -5.14
-1.21 -2.01 -2.00
Re = 14 kpc Re = 19 kpc Re = 11 kpc
A V (d
ex)
0.00.51.01.52.02.53.03.54.0
0.0
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)
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A7. Comparison of the AGN with MaNGA ID 1-148068 and its control galaxies.
9SD
SS Im
age
1-149211 1-377321 1-491233
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.08 0.15 -0.24
-0.15 -0.00 0.13
-0.12 0.07 -0.09
0.00 -4.25 -1.92
0.00 -7.44 -1.27
0.00 -6.34 -1.63
1.65 12.97 27.19
5.44 8.47 7.75
3.22 11.90 27.75
-2.52 -0.17 -31.01
-2.56 7.74 -9.53
-2.52 2.77 -29.22
-0.01 0.13 -0.26
-0.04 0.42 -0.18
-0.01 0.28 -0.33
Re = 2.7 kpc Re = 2.6 kpc Re = 3.0 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.41.6
0.0
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1.0
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(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A8. Comparison of the AGN with MaNGA ID 1-149211 and its control galaxies.
10SD
SS Im
age
1-163831 1-247456 1-210593
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.21 0.01 -0.21
0.06 -1.90 0.30
0.09 0.05 0.04
6.62 1.44 0.21
2.06 59.70 5.00
8.07 5.60 2.09
42.82 57.76 -1.35
37.65 -127.70 45.16
56.66 42.88 21.73
-55.22 -98.88 0.87
-50.22 175.75 -54.13
-71.78 -82.66 -25.92
-0.89 -3.37 -0.01
-0.78 5.04 -0.79
-1.17 -2.83 -0.37
Re = 8.9 kpc Re = 15 kpc Re = 6.8 kpc
A V (d
ex)
0.000.250.500.751.001.251.501.752.00
0.1
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0.3
0.4
0.5
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A9. Comparison of the AGN with MaNGA ID 1-163831 and its control galaxies.
11SD
SS Im
age
1-166919 12-129446 1-90849
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.25 0.30 0.35
0.26 -0.18 0.03
0.28 0.10 0.17
5.60 8.08 7.14
7.87 -0.49 5.54
7.48 5.51 7.93
13.14 39.77 53.34
26.39 38.04 21.17
20.90 38.78 46.87
-15.66 -49.35 -56.54
-33.21 -49.50 -35.17
-26.09 -50.90 -55.16
-0.41 -0.87 -0.91
-0.65 -0.67 -0.80
-0.58 -0.85 -0.96
Re = 6.4 kpc Re = 7.1 kpc Re = 7.6 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
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0.5
0.1
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(%)
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)
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A10. Comparison of the AGN with MaNGA ID 1-166919 and its control galaxies.
12SD
SS Im
age
1-167688 1-235587 1-37062
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.15 0.01 -0.55
0.03 0.01 -1.53
0.05 0.01 -0.68
-6.42 0.16 -7.02
-2.13 0.34 -23.68
-4.56 0.10 -12.76
-27.04 6.10 -14.32
-41.40 3.01 -79.10
-23.53 5.76 -10.75
29.36 -8.63 26.44
7.92 -8.63 -40.37
17.61 -9.88 15.99
0.51 -0.08 0.42
-4.23 -0.11 -14.42
-0.82 -0.09 -0.81
Re = 2.8 kpc Re = 2.8 kpc Re = 4.0 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
0.0
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)
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A11. Comparison of the AGN with MaNGA ID 1-167688 and its control galaxies.
13SD
SS Im
age
1-173958 1-247456 1-24246
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-1.34 0.01 0.02
0.76 -1.90 1.04
-0.92 0.05 0.77
-20.00 1.44 0.00
16.15 59.70 -0.12
-11.23 5.60 0.08
55.87 57.76 47.88
93.49 -127.70 72.39
58.18 42.88 76.21
-24.84 -98.88 -69.01
-187.98 175.75 -38.87
-49.93 -82.66 -73.92
-0.23 -3.37 -1.35
-14.89 5.04 0.37
-1.75 -2.83 -1.04
Re = 15 kpc Re = 15 kpc Re = 8.9 kpc
A V (d
ex)
0.000.250.500.751.001.251.501.752.00
0.0
0.2
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0.6
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)
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A12. Comparison of the AGN with MaNGA ID 1-173958 and its control galaxies.
14SD
SS Im
age
1-198153 1-211063 1-135810
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.55 -0.18 -0.26
0.61 -0.01 0.33
0.09 -0.11 0.21
-0.15 6.99 5.15
9.21 9.86 9.56
4.71 9.01 9.39
52.47 72.50 0.24
46.68 -22.10 53.83
60.63 75.45 30.09
-52.36 -91.47 -12.22
-73.53 -27.92 -62.22
-71.42 -101.90 -41.46
-0.55 -1.25 -0.31
-2.59 -1.46 -0.96
-1.36 -1.70 -0.75
Re = 9.2 kpc Re = 11 kpc Re = 6.8 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.7
0.0
0.1
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(%)
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<t [l
og(y
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8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A13. Comparison of the AGN with MaNGA ID 1-198153 and its control galaxies.
15SD
SS Im
age
1-198182 1-256185 1-48053
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.00 -0.03 0.00
0.36 0.24 0.01
0.10 0.10 0.00
-0.37 0.00 -0.12
3.52 -0.02 0.00
0.86 0.01 -0.05
27.28 35.96 0.95
-1.65 -0.42 7.60
11.34 29.80 3.12
-27.13 -36.55 -1.13
-23.11 -11.01 -14.73
-18.96 -33.63 -4.52
-0.27 -0.37 -0.04
-2.18 -1.28 -0.82
-0.76 -0.67 -0.22
Re = 6.9 kpc Re = 5.9 kpc Re = 9.5 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.41.6
0.0
0.1
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0.3
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(%)
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A14. Comparison of the AGN with MaNGA ID 1-198182 and its control galaxies.
16SD
SS Im
age
1-201561 1-24246 1-285052
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.06 0.02 -0.31
--- 1.04 0.06
0.06 0.77 -0.09
10.30 0.00 0.73
--- -0.12 -0.18
10.30 0.08 0.22
28.67 47.88 32.29
--- 72.39 37.86
28.67 76.21 31.76
-66.43 -69.01 -32.92
--- -38.87 -60.54
-66.43 -73.92 -41.39
-3.43 -1.35 -0.38
--- 0.37 -0.89
-3.43 -1.04 -0.61
Re = 16 kpc Re = 8.9 kpc Re = 8.5 kpc
A V (d
ex)
0.0
0.2
0.4
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1.2
0.0
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(%)
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og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A15. Comparison of the AGN with MaNGA ID 1-201561 and its control galaxies.
17SD
SS Im
age
1-209980 1-295095 1-92626
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.01 0.04 -0.13
-0.00 0.03 ---
-0.06 0.05 -0.13
5.01 0.00 10.52
-4.57 2.43 ---
0.12 0.86 10.52
15.01 -5.22 38.76
56.89 33.62 ---
27.14 16.40 38.76
-3.05 -5.38 -63.62
-53.38 -46.80 ---
-18.65 -29.29 -63.62
-0.36 -0.03 -2.22
-0.45 -0.63 ---
-0.30 -0.36 -2.22
Re = 4.7 kpc Re = 2.7 kpc Re = 13 kpc
A V (d
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0.0
0.2
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A16. Comparison of the AGN with MaNGA ID 1-209980 and its control galaxies.
18SD
SS Im
age
1-210646 1-114306 1-487130
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.03 -0.79 -0.35
-0.17 -0.00 -0.18
-0.04 -0.10 -0.27
6.28 -9.70 12.25
5.54 23.40 -4.18
4.92 9.99 7.04
38.02 43.55 11.46
30.68 -29.96 -45.14
37.67 9.84 11.14
-41.48 -44.17 -14.22
-41.13 -1.38 -17.21
-49.12 -23.34 -33.58
-0.75 -0.12 -0.61
-1.04 -1.44 -6.16
-0.88 -0.83 -2.31
Re = 10.0 kpc Re = 11 kpc Re = 8.2 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.4
0.2
0.4
0.6
0.8
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(%)
0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A17. Comparison of the AGN with MaNGA ID 1-210646 and its control galaxies.
19SD
SS Im
age
1-211311 1-25688 1-94422
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.09 -0.27 0.05
-0.01 -0.12 -0.48
-0.02 -0.19 0.08
0.55 3.42 2.30
0.66 -1.29 2.91
0.40 3.11 1.97
52.34 -5.63 50.14
61.72 28.41 46.27
60.60 14.95 52.89
-47.60 -2.16 -61.80
-86.83 -36.48 -181.64
-70.14 -25.98 -73.82
-0.56 -0.16 -1.05
-1.72 -0.50 -10.95
-0.98 -0.46 -1.82
Re = 4.2 kpc Re = 4.3 kpc Re = 7.8 kpc
A V (d
ex)
0.0
0.1
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<t [l
og(y
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8.0
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9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A18. Comparison of the AGN with MaNGA ID 1-211311 and its control galaxies.
20SD
SS Im
age
1-217050 1-135372 1-274663
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.02 -0.00 -0.41
0.05 0.00 0.11
0.02 0.00 -0.05
0.10 -0.01 0.22
-0.01 0.00 0.07
-0.02 -0.00 0.91
6.25 26.86 10.70
12.70 26.23 4.95
8.06 25.02 6.77
-7.40 -23.73 -11.09
-11.83 -34.77 -7.14
-8.05 -26.51 -8.38
-0.05 -0.26 -0.12
-0.16 -1.07 -0.25
-0.09 -0.48 -0.15
Re = 4.8 kpc Re = 6.5 kpc Re = 6.4 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.7
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
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50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
40
60
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100
0
20
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A19. Comparison of the AGN with MaNGA ID 1-217050 and its control galaxies.
21SD
SS Im
age
1-22301 1-251871 1-72914
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.48 0.10 0.13
0.25 -0.34 ---
-0.05 0.13 0.13
0.55 2.54 7.18
26.63 1.33 ---
10.86 1.07 7.18
31.33 36.12 53.49
20.95 15.96 ---
33.54 55.75 53.49
-43.02 -46.76 -99.37
-48.17 -146.68 ---
-58.18 -85.53 -99.37
-0.57 -0.81 -5.64
-1.99 -12.52 ---
-1.38 -2.82 -5.64
Re = 11 kpc Re = 18 kpc Re = 21 kpc
A V (d
ex)
0.000.050.100.150.200.250.300.350.40
0.10
0.15
0.20
0.25
0.30
0.35
x yy +
xyo
(%)
0
10
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30
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50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
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100
0
20
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60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A20. Comparison of the AGN with MaNGA ID 1-22301 and its control galaxies.
22SD
SS Im
age
1-229010 1-210962 1-613211
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.20 0.06 0.07
--- 0.23 0.25
0.20 0.13 0.29
3.21 0.02 0.12
--- 0.34 -0.26
3.21 0.07 -0.13
133.88 61.83 -2.41
--- 22.34 4.11
133.88 46.69 3.45
-200.54 -63.42 1.73
--- -28.06 -3.69
-200.54 -48.96 -3.16
-3.30 -0.59 0.04
--- -0.90 -0.03
-3.30 -0.64 -0.03
Re = 27 kpc Re = 8.7 kpc Re = 4.5 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.7
0.0
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
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50
x iy +
xii +
xio
(%)
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x o (%
)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A21. Comparison of the AGN with MaNGA ID 1-229010 and its control galaxies.
23SD
SS Im
age
1-234618 1-282144 1-339125
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.48 -0.03 0.60
0.25 -1.01 -0.24
0.31 -0.52 0.10
8.10 3.11 1.83
4.53 5.05 -0.21
6.41 0.82 1.77
35.88 56.09 26.61
-18.95 -25.88 -0.36
25.65 19.53 14.42
-39.78 -48.60 -28.48
-4.09 -5.73 0.64
-35.31 -32.67 -16.32
-0.69 -0.70 -0.41
-1.95 -2.12 0.02
-1.31 -1.60 -0.23
Re = 19 kpc Re = 12 kpc Re = 5.9 kpc
A V (d
ex)
0.0
0.5
1.0
1.5
2.0
2.5
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
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100
x o (%
)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A22. Comparison of the AGN with MaNGA ID 1-234618 and its control galaxies.
24SD
SS Im
age
1-23979 1-320681 1-519738
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.02 0.00 0.00
-0.24 0.00 0.00
-0.17 0.00 0.00
2.05 0.00 0.00
-4.68 0.00 0.00
-2.29 -0.00 0.00
0.38 0.25 19.29
7.56 6.48 29.56
8.77 3.46 38.86
0.31 -0.25 -18.18
-4.92 -7.49 -29.56
-6.07 -3.78 -38.33
-0.06 0.01 -0.19
0.06 -0.10 -0.23
-0.02 -0.04 -0.36
Re = 3.1 kpc Re = 2.5 kpc Re = 3.1 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
0.0
0.2
0.4
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A23. Comparison of the AGN with MaNGA ID 1-23979 and its control galaxies.
25SD
SS Im
age
1-24148 1-285031 1-236099
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.16 -0.27 -0.35
-0.22 0.23 -0.15
-0.27 0.01 -0.39
0.10 3.43 -3.26
-0.22 6.01 1.04
0.01 5.86 -1.94
8.03 26.35 -14.33
18.87 29.15 -3.20
10.34 32.47 -2.12
-6.79 -31.48 12.52
-18.84 -36.46 0.34
-9.13 -39.55 1.54
-0.10 -0.43 0.32
-0.20 -0.63 -0.64
-0.12 -0.62 -0.07
Re = 3.6 kpc Re = 3.3 kpc Re = 2.7 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.2
0.4
0.6
0.8
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xyo
(%)
0
10
20
30
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50
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xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A24. Comparison of the AGN with MaNGA ID 1-24148 and its control galaxies.
26SD
SS Im
age
1-248389 1-94554 1-245774
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.65 0.01 0.70
0.00 0.60 0.01
-0.42 0.10 0.38
-1.56 0.44 15.42
-0.00 5.71 7.31
-1.00 1.58 11.32
74.05 9.00 68.32
-110.71 23.57 35.39
37.41 9.13 58.50
-70.90 -8.55 -83.55
5.12 -160.21 -49.66
-48.67 -23.66 -74.89
-0.35 -0.13 -1.47
-9.91 -14.24 -1.31
-1.59 -1.46 -1.37
Re = 7.6 kpc Re = 5.2 kpc Re = 7.2 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
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50
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xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A25. Comparison of the AGN with MaNGA ID 1-248389 and its control galaxies.
27SD
SS Im
age
1-248420 1-211063 1-211074
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.12 -0.18 -0.13
0.01 -0.01 ---
0.01 -0.11 -0.13
8.69 6.99 2.46
7.46 9.86 ---
11.19 9.01 2.46
27.05 72.50 166.90
44.81 -22.10 ---
57.19 75.45 166.90
-51.38 -91.47 -191.75
-66.84 -27.92 ---
-81.44 -101.90 -191.75
-0.84 -1.25 -3.87
-1.98 -1.46 ---
-1.63 -1.70 -3.87
Re = 6.7 kpc Re = 11 kpc Re = 33 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.70.8
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A26. Comparison of the AGN with MaNGA ID 1-248420 and its control galaxies.
28SD
SS Im
age
1-25554 1-135625 1-216958
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.09 -0.40 -0.12
-0.26 -0.47 -0.29
-0.09 -0.47 -0.14
0.07 -15.67 -4.46
7.43 -1.46 -4.53
5.52 -9.69 -1.07
47.46 -2.66 14.03
2.82 21.72 5.09
37.19 2.04 25.16
-42.11 34.33 -15.57
-42.67 -38.92 -49.48
-56.65 6.39 -45.32
-0.52 0.81 -0.04
-2.09 -0.49 -3.61
-1.26 0.26 -1.16
Re = 8.5 kpc Re = 3.4 kpc Re = 5.5 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A27. Comparison of the AGN with MaNGA ID 1-25554 and its control galaxies.
29SD
SS Im
age
1-256446 1-322671 1-256465
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.67 0.03 0.20
-0.04 0.00 -0.03
-0.34 0.01 0.09
0.00 0.12 4.03
0.00 -0.02 -2.63
0.00 0.04 1.81
26.42 15.96 22.67
20.16 -20.50 39.24
35.91 3.02 24.49
-30.60 -15.99 -23.20
-43.63 12.00 -93.94
-45.07 -5.38 -37.79
-0.25 -0.15 -0.26
-2.85 -0.63 -5.88
-1.13 -0.27 -1.49
Re = 6.5 kpc Re = 5.3 kpc Re = 6.6 kpc
A V (d
ex)
0.000.050.100.150.200.250.300.35
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
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60
80
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A28. Comparison of the AGN with MaNGA ID 1-256446 and its control galaxies.
30SD
SS Im
age
1-25725 1-211079 1-322074
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.51 0.00 0.05
-0.20 0.00 0.04
-0.28 0.00 0.02
0.00 0.00 0.00
0.19 0.00 0.00
0.05 0.00 0.00
33.29 4.43 9.95
-7.79 14.71 11.32
34.52 10.47 12.13
-38.87 -4.82 -10.76
-23.90 -14.19 -12.06
-42.07 -10.59 -12.46
-0.40 -0.06 -0.09
-4.23 -0.23 -0.23
-1.22 -0.13 -0.15
Re = 4.4 kpc Re = 2.2 kpc Re = 2.2 kpc
A V (d
ex)
0.00.20.40.60.81.01.2
0.0
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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100
x o (%
)
0
20
40
60
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100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A29. Comparison of the AGN with MaNGA ID 1-25725 and its control galaxies.
31SD
SS Im
age
1-258599 1-93876 1-166691
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.15 0.07 -0.01
-0.93 -0.13 -0.03
-0.54 0.09 -0.03
-6.39 0.00 1.16
-29.52 0.00 -1.84
-15.73 0.00 -0.80
46.64 -0.07 -2.06
38.71 -47.44 18.13
68.52 3.36 6.18
-18.88 -2.34 -1.67
-63.15 -80.64 -19.72
-47.26 -21.76 -8.76
-0.14 -0.14 -0.01
-3.83 -12.97 -0.16
-0.89 -1.85 -0.05
Re = 14 kpc Re = 12 kpc Re = 4.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
0.0
0.2
0.4
0.6
0.8
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xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
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)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A30. Comparison of the AGN with MaNGA ID 1-258599 and its control galaxies.
32SD
SS Im
age
1-258774 1-379660 1-48208
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.08 -0.05 0.00
-0.02 -0.22 -0.02
-0.02 -0.17 -0.00
0.51 0.94 0.03
0.99 0.67 -0.00
-0.46 0.91 -0.01
0.93 26.73 36.18
-10.84 -6.42 -76.41
-9.12 16.26 22.05
1.26 -28.61 -37.26
7.25 1.99 -9.05
9.39 -19.99 -34.52
-0.02 -0.19 -0.38
-0.26 -0.05 -8.22
0.03 -0.15 -1.49
Re = 4.3 kpc Re = 2.9 kpc Re = 7.6 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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x o (%
)
0
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A31. Comparison of the AGN with MaNGA ID 1-258774 and its control galaxies.
33SD
SS Im
age
1-259142 1-55572 1-489649
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.21 0.20 -0.29
1.31 0.17 0.21
0.33 0.36 -0.06
2.05 2.76 -0.65
5.17 14.67 0.64
1.73 9.14 -0.22
68.65 44.77 15.56
40.72 -5.17 19.47
70.56 54.71 18.18
-82.29 -45.91 -13.88
-329.86 -60.90 -19.87
-91.34 -76.95 -17.06
-1.62 -0.68 -0.14
-27.91 -5.14 -0.26
-2.10 -2.00 -0.22
Re = 19 kpc Re = 11 kpc Re = 6.7 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.7
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A32. Comparison of the AGN with MaNGA ID 1-259142 and its control galaxies.
34SD
SS Im
age
1-269632 1-210700 1-378795
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.08 -0.01 0.20
-0.50 --- 0.35
-0.30 -0.01 0.32
-18.37 0.01 -1.34
-4.98 --- 2.97
-15.17 0.01 1.57
50.81 14.19 50.97
19.31 --- 38.81
43.17 14.19 45.41
-12.62 -51.47 -56.13
-22.80 --- -56.99
-20.69 -51.47 -56.83
0.29 -5.03 -0.59
-0.91 --- -1.50
-0.08 -5.03 -0.92
Re = 13 kpc Re = 25 kpc Re = 12 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.70.8
0.0
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A33. Comparison of the AGN with MaNGA ID 1-269632 and its control galaxies.
35SD
SS Im
age
1-277552 1-264513 1-136125
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.09 -0.21 -0.35
-0.49 -0.05 -0.20
-0.29 -0.10 -0.05
16.67 11.62 11.61
6.93 18.36 4.10
11.10 15.91 9.12
51.64 -18.35 -11.04
14.51 -28.33 45.32
33.62 -6.19 28.08
-80.37 -15.97 -2.28
-33.83 -6.11 -54.31
-54.39 -25.13 -41.19
-1.50 -0.79 -0.38
-0.61 -1.12 -1.20
-1.04 -1.15 -0.92
Re = 13 kpc Re = 10 kpc Re = 9.0 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
0.2
0.4
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
40
60
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100
0
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60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A34. Comparison of the AGN with MaNGA ID 1-277552 and its control galaxies.
36SD
SS Im
age
1-279073 1-211100 1-210784
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.00 0.00 -0.26
0.02 0.03 0.01
0.03 0.01 -0.09
0.60 0.00 0.04
-0.33 0.22 -0.06
0.16 0.06 0.00
36.56 5.25 -8.79
68.34 31.01 0.33
39.65 18.68 -2.52
-38.44 -5.37 9.67
-89.11 -42.29 -0.08
-46.86 -22.53 3.10
-0.49 -0.08 0.15
-3.29 -1.40 -0.01
-1.14 -0.57 0.05
Re = 5.6 kpc Re = 3.8 kpc Re = 4.3 kpc
A V (d
ex)
0.000.050.100.150.200.250.30
0.00
0.02
0.04
0.06
0.08
0.10
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A35. Comparison of the AGN with MaNGA ID 1-279073 and its control galaxies.
37SD
SS Im
age
1-279147 1-283246 1-351538
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.75 0.13 -1.19
-0.44 0.05 ---
-0.63 0.09 -1.19
3.39 0.67 -0.07
-3.27 -0.98 ---
0.88 -0.47 -0.07
24.07 9.85 46.74
-22.98 28.78 ---
3.89 18.92 46.74
-16.62 -10.42 -73.41
-19.12 -28.87 ---
-9.41 -18.94 -73.41
-0.18 -0.20 -3.30
-3.84 -0.21 ---
-0.97 -0.20 -3.30
Re = 5.8 kpc Re = 4.7 kpc Re = 18 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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x o (%
)
0
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60
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100
0
20
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A36. Comparison of the AGN with MaNGA ID 1-279147 and its control galaxies.
38SD
SS Im
age
1-279666 1-392976 1-47499
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.01 0.04 0.02
0.01 0.09 -0.46
-0.01 0.07 -0.21
-0.33 0.00 1.19
0.44 0.00 -0.73
0.24 0.00 0.38
6.00 -5.06 -7.92
7.63 -7.83 -2.70
7.01 -7.69 -5.13
-5.67 5.27 6.73
-8.07 6.84 2.16
-7.25 7.18 4.36
-0.04 0.03 0.06
-0.12 0.06 0.05
-0.09 0.06 0.08
Re = 2.1 kpc Re = 1.6 kpc Re = 3.1 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
40
60
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0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A37. Comparison of the AGN with MaNGA ID 1-279666 and its control galaxies.
39SD
SS Im
age
1-279676 1-44789 1-378401
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.35 -0.08 -0.00
-0.05 0.19 0.00
0.21 -0.07 -0.00
2.89 0.00 0.07
1.70 0.00 -0.28
5.05 0.00 0.05
27.66 3.52 1.09
15.16 40.06 3.30
39.27 18.07 4.26
-32.71 -4.47 0.79
-35.03 -65.06 -1.31
-52.63 -27.53 -1.94
-0.46 -0.01 -0.01
-1.34 -3.13 -0.05
-1.10 -1.00 -0.06
Re = 7.5 kpc Re = 7.8 kpc Re = 5.1 kpc
A V (d
ex)
0.0
0.5
1.0
1.5
2.0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
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40
60
80
100
0
20
40
60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A38. Comparison of the AGN with MaNGA ID 1-279676 and its control galaxies.
40SD
SS Im
age
1-321739 1-247417 1-633994
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.22 0.26 -0.78
-0.20 0.38 -0.01
-0.23 0.32 -0.30
2.81 15.73 2.32
9.64 7.65 -0.11
4.06 9.74 5.11
86.58 13.03 58.90
-9.29 14.82 37.87
39.82 21.69 40.25
-91.57 -22.56 -61.53
-24.20 -25.30 -59.91
-55.85 -30.98 -52.50
-1.13 -0.78 -0.74
-0.56 -0.54 -2.58
-0.76 -0.69 -1.28
Re = 7.1 kpc Re = 5.9 kpc Re = 7.2 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.41.6
0.6
0.8
1.0
1.2
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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60
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A39. Comparison of the AGN with MaNGA ID 1-321739 and its control galaxies.
41SD
SS Im
age
1-338922 1-286804 1-109493
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.54 0.26 -0.01
-1.04 -0.14 ---
-0.10 -0.06 -0.01
-3.04 1.67 -3.80
-0.00 18.73 ---
-1.85 -2.15 -3.80
-24.39 -96.44 58.95
5.13 78.41 ---
0.29 -6.85 58.95
42.70 68.94 -119.90
4.65 -104.08 ---
16.56 -17.07 -119.90
0.43 0.63 -8.32
0.27 -1.89 ---
0.35 -0.33 -8.32
Re = 24 kpc Re = 43 kpc Re = 40 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.70.8
0.0
0.2
0.4
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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60
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A40. Comparison of the AGN with MaNGA ID 1-338922 and its control galaxies.
42SD
SS Im
age
1-339094 1-274646 1-24099
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.54 -0.38 0.02
-0.32 -0.15 0.08
-0.52 -0.38 0.07
1.34 -0.42 0.17
-1.29 0.03 0.51
0.31 -0.08 0.79
13.33 13.47 11.55
-10.86 -5.76 30.67
2.23 5.93 18.49
-16.23 -11.92 -14.08
12.43 6.99 -30.96
-3.64 -4.17 -19.30
-0.20 -0.08 -0.14
0.11 -0.02 -0.33
-0.06 -0.03 -0.25
Re = 2.6 kpc Re = 2.7 kpc Re = 2.1 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.4
0.0
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A41. Comparison of the AGN with MaNGA ID 1-339094 and its control galaxies.
43SD
SS Im
age
1-339163 1-136125 1-626830
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.11 -0.35 -0.85
0.49 -0.20 0.07
0.41 -0.05 -0.19
1.20 11.61 -0.37
7.24 4.10 4.81
5.53 9.12 2.39
60.28 -11.04 -9.09
35.98 45.32 40.95
64.15 28.08 20.65
-64.57 -2.28 7.15
-76.69 -54.31 -47.90
-84.95 -41.19 -26.39
-0.78 -0.38 0.24
-3.11 -1.20 -0.61
-1.76 -0.92 -0.33
Re = 9.9 kpc Re = 9.0 kpc Re = 5.7 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.70.8
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
20
40
60
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100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A42. Comparison of the AGN with MaNGA ID 1-339163 and its control galaxies.
44SD
SS Im
age
1-351790 1-23731 1-167334
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.05 -0.22 -0.27
-0.28 0.10 -0.50
-0.28 -0.04 -0.45
6.75 -1.89 4.22
-3.95 -0.00 -4.05
2.26 -0.99 -0.22
-25.51 -1.86 -17.72
-24.63 13.24 -20.13
-35.60 7.45 -18.44
19.43 0.23 13.50
26.68 -13.61 20.16
31.52 -8.33 17.15
-0.01 -0.08 0.02
0.34 -0.17 0.46
0.20 -0.17 0.25
Re = 2.2 kpc Re = 1.9 kpc Re = 1.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A43. Comparison of the AGN with MaNGA ID 1-351790 and its control galaxies.
45SD
SS Im
age
1-37036 1-210785 1-25680
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.40 -0.37 -0.02
-0.55 -0.02 -0.00
-0.27 -0.11 -0.01
-0.01 -0.49 0.00
-0.12 0.07 0.00
-0.00 -0.19 0.00
40.51 51.17 6.95
-79.23 -18.08 -9.06
24.39 18.87 5.13
-37.18 -50.83 -4.64
-135.19 8.09 -53.76
-35.44 -21.77 -13.22
-0.58 -0.45 -0.11
-21.00 -0.81 -6.37
-1.71 -0.46 -1.04
Re = 9.6 kpc Re = 7.0 kpc Re = 6.8 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A44. Comparison of the AGN with MaNGA ID 1-37036 and its control galaxies.
46SD
SS Im
age
1-373161 1-259650 1-289865
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.23 0.06 -0.00
--- 9.68 -0.00
-0.23 0.38 -0.00
0.17 0.23 0.16
--- 95.34 0.40
0.17 1.83 0.14
10.64 9.12 21.76
--- 62.76 45.04
10.64 8.67 22.18
-5.81 -20.76 -28.63
--- -109.16 -130.55
-5.81 -24.66 -33.22
-0.13 -1.50 -0.24
--- 6.45 -9.56
-0.13 -1.55 -0.99
Re = 27 kpc Re = 25 kpc Re = 17 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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100
x o (%
)
0
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0
20
40
60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A45. Comparison of the AGN with MaNGA ID 1-373161 and its control galaxies.
47SD
SS Im
age
1-44303 1-339028 1-379087
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.17 0.05 -1.29
0.09 --- -0.05
-0.14 0.05 -0.66
9.56 3.25 -5.86
9.95 --- 10.95
9.54 3.25 5.89
31.22 44.37 -15.80
38.93 --- 47.52
30.85 44.37 16.63
-27.11 -67.95 21.74
-77.05 --- -78.80
-44.57 -67.95 -29.94
-0.81 -2.67 0.42
-3.43 --- -3.13
-1.71 -2.67 -1.10
Re = 7.8 kpc Re = 19 kpc Re = 8.4 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
0.0
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
10
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40
50
x iy +
xii +
xio
(%)
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100
x o (%
)
0
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100
0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A46. Comparison of the AGN with MaNGA ID 1-44303 and its control galaxies.
48SD
SS Im
age
1-44379 1-211082 1-135371
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.55 0.23 -0.30
0.18 -0.06 0.50
0.47 0.20 0.15
17.43 5.85 2.61
7.57 4.14 11.17
15.91 5.65 8.83
49.45 21.40 35.64
18.47 10.02 28.29
33.71 23.83 28.80
-58.84 -30.36 -38.25
-27.27 -14.84 -39.61
-46.93 -30.19 -37.76
-1.24 -0.53 -0.52
-0.58 -0.27 -0.83
-1.08 -0.52 -0.71
Re = 5.8 kpc Re = 7.1 kpc Re = 5.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
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40
50
x iy +
xii +
xio
(%)
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x o (%
)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A47. Comparison of the AGN with MaNGA ID 1-44379 and its control galaxies.
49SD
SS Im
age
1-460812 1-270160 1-258455
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.47 -0.62 -0.85
-0.33 -0.06 0.16
-0.51 -0.42 -0.36
-0.13 -0.18 -3.68
-0.40 -0.02 0.25
-0.50 -0.13 -1.65
27.22 4.88 13.51
35.45 2.92 -44.45
31.21 1.32 3.58
-26.70 -5.36 -11.71
-32.43 -1.53 25.30
-30.39 -2.39 -8.06
-0.26 -0.05 0.03
-0.27 -0.07 -1.94
-0.24 -0.02 -0.53
Re = 7.0 kpc Re = 8.5 kpc Re = 10 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
0.0
0.2
0.4
0.6
0.8
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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x o (%
)
0
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A48. Comparison of the AGN with MaNGA ID 1-460812 and its control galaxies.
50SD
SS Im
age
1-48116 1-386452 1-24416
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.47 -0.15 -0.51
0.02 -0.31 0.13
-0.18 -0.27 -0.12
0.41 -6.35 0.01
7.71 -2.94 0.42
5.32 -7.85 0.25
-12.34 40.30 13.93
34.87 -3.08 41.98
18.31 18.84 25.76
13.83 -34.57 -14.22
-48.25 -6.43 -44.45
-24.96 -15.69 -26.73
0.10 -0.21 -0.12
-0.77 -1.32 -0.50
-0.44 -0.31 -0.31
Re = 4.3 kpc Re = 4.5 kpc Re = 4.3 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
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x iy +
xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A49. Comparison of the AGN with MaNGA ID 1-48116 and its control galaxies.
51SD
SS Im
age
1-491229 1-94554 1-604048
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.16 0.01 0.28
0.27 0.60 -0.26
0.00 0.10 0.12
1.84 0.44 11.71
0.75 5.71 -12.42
1.49 1.58 11.68
13.41 9.00 27.62
9.03 23.57 -47.66
12.50 9.13 15.61
-13.10 -8.55 -41.34
-66.73 -160.21 -25.96
-24.21 -23.66 -43.12
-0.20 -0.13 -0.89
-5.80 -14.24 -7.76
-1.31 -1.46 -2.32
Re = 7.8 kpc Re = 5.2 kpc Re = 12 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.0
0.1
0.2
0.3
x yy +
xyo
(%)
0
10
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50
x iy +
xii +
xio
(%)
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x o (%
)
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0
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A50. Comparison of the AGN with MaNGA ID 1-491229 and its control galaxies.
52SD
SS Im
age
1-519742 1-37079 1-276679
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.08 0.05 -0.04
-0.07 -0.22 -0.31
-0.09 -0.02 -0.11
0.01 3.96 7.36
-0.07 -16.78 -8.02
0.16 2.06 1.86
-7.37 -33.49 -27.78
25.78 -16.31 25.44
12.23 -33.15 9.77
0.53 28.23 18.39
-53.69 -0.71 -34.18
-24.21 20.60 -16.10
-0.10 -0.11 -0.01
-3.20 -1.70 -1.33
-1.06 -0.92 -0.56
Re = 2.6 kpc Re = 2.3 kpc Re = 3.6 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.0
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
10
20
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xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A51. Comparison of the AGN with MaNGA ID 1-519742 and its control galaxies.
53SD
SS Im
age
1-542318 1-285052 1-377125
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.23 -0.31 -0.33
0.00 0.06 -1.00
-0.11 -0.09 -0.31
0.00 0.73 7.17
5.29 -0.18 -23.46
1.62 0.22 5.59
13.96 32.29 72.35
-11.85 37.86 30.08
8.45 31.76 75.26
-5.45 -32.92 -95.35
1.08 -60.54 -88.42
-10.63 -41.39 -106.28
-0.17 -0.38 -1.18
-0.84 -0.89 -7.40
-0.62 -0.61 -1.86
Re = 9.4 kpc Re = 8.5 kpc Re = 13 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.41.6
0.00
0.05
0.10
0.15
0.20
0.25
0.30
x yy +
xyo
(%)
0
10
20
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50
x iy +
xii +
xio
(%)
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)
0
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A52. Comparison of the AGN with MaNGA ID 1-542318 and its control galaxies.
54SD
SS Im
age
1-558912 1-71481 1-72928
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.22 0.17 0.00
--- --- 0.00
-0.22 0.17 0.00
0.83 0.37 0.00
--- --- 0.00
0.83 0.37 0.00
36.10 31.08 17.36
--- --- 348.08
36.10 31.08 33.16
-21.42 -64.82 -27.74
--- --- -257.25
-21.42 -64.82 -39.79
-6.85 -4.71 -0.84
--- --- 4.05
-6.85 -4.71 -0.74
Re = 68 kpc Re = 46 kpc Re = 16 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.000
0.025
0.050
0.075
0.100
0.125
0.150
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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x o (%
)
0
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40
60
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100
0
20
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A53. Comparison of the AGN with MaNGA ID 1-558912 and its control galaxies.
55SD
SS Im
age
1-604761 1-210173 1-71525
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.19 0.41 -0.97
--- 0.78 0.25
-0.19 0.37 -0.02
2.51 18.35 1.75
--- 19.67 22.88
2.51 17.83 14.85
125.86 58.39 74.96
--- 0.56 -1.15
125.86 64.18 37.53
-151.19 -78.86 -77.12
--- -92.99 -30.63
-151.19 -93.81 -55.48
-3.86 -1.74 -0.79
--- -9.93 -1.64
-3.86 -2.71 -1.26
Re = 35 kpc Re = 17 kpc Re = 7.9 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
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50
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xii +
xio
(%)
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)
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0
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<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A54. Comparison of the AGN with MaNGA ID 1-604761 and its control galaxies.
56SD
SS Im
age
1-72322 1-121717 1-43721
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.15 -0.78 -0.27
-0.76 --- ---
-0.10 -0.78 -0.27
3.31 8.53 -1.80
-4.91 --- ---
0.45 8.53 -1.80
38.19 60.73 0.93
59.98 --- ---
47.24 60.73 0.93
-32.46 -83.57 -18.64
-47.85 --- ---
-43.43 -83.57 -18.64
-0.70 -3.77 -2.44
0.67 --- ---
-0.75 -3.77 -2.44
Re = 22 kpc Re = 32 kpc Re = 26 kpc
A V (d
ex)
0.00.10.20.30.40.50.60.70.8
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
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x o (%
)
0
20
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60
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0
20
40
60
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100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A55. Comparison of the AGN with MaNGA ID 1-72322 and its control galaxies.
57SD
SS Im
age
1-91016 1-338828 1-386695
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.39 -0.07 0.22
-0.26 -0.08 -0.27
-0.45 -0.10 -0.05
-0.79 -2.45 -11.62
2.04 1.59 -18.34
-0.46 -0.99 -16.92
10.86 -13.16 54.60
33.55 7.61 47.21
22.38 -2.26 60.22
-12.92 9.82 -22.38
-40.22 -4.00 -19.05
-27.79 1.11 -25.79
-0.15 0.12 0.16
-0.58 -0.18 0.28
-0.34 -0.02 0.20
Re = 4.2 kpc Re = 3.5 kpc Re = 4.6 kpc
A V (d
ex)
0.000.250.500.751.001.251.501.75
0.4
0.6
0.8
1.0
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
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100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A56. Comparison of the AGN with MaNGA ID 1-91016 and its control galaxies.
58SD
SS Im
age
1-92866 1-94514 1-210614
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.09 0.00 0.02
--- -0.01 ---
-0.09 0.00 0.02
0.00 1.26 0.12
--- 5.50 ---
0.00 2.75 0.12
111.45 1.56 29.09
--- 29.70 ---
111.45 1.25 29.09
-110.31 -2.22 -55.14
--- 76.61 ---
-110.31 2.37 -55.14
-2.23 -0.15 -2.91
--- 10.48 ---
-2.23 0.32 -2.91
Re = 21 kpc Re = 14 kpc Re = 26 kpc
A V (d
ex)
0.0000.0250.0500.0750.1000.1250.1500.175
0.00
0.02
0.04
0.06
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
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80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A57. Comparison of the AGN with MaNGA ID 1-92866 and its control galaxies.
59SD
SS Im
age
1-94604 1-295095 1-134239
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.06 0.04 0.30
-0.16 0.03 -0.34
-0.05 0.05 0.13
4.68 0.00 12.30
-5.19 2.43 15.96
1.97 0.86 12.07
-19.84 -5.22 52.68
28.00 33.62 -106.17
24.09 16.40 38.96
22.02 -5.38 -74.56
-120.16 -46.80 -108.85
-50.56 -29.29 -89.82
-0.36 -0.03 -1.32
-8.34 -0.63 -22.88
-2.73 -0.36 -4.23
Re = 5.0 kpc Re = 2.7 kpc Re = 11 kpc
A V (d
ex)
0.0
0.1
0.2
0.3
0.4
0.5
0.00
0.05
0.10
0.15
0.20
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A58. Comparison of the AGN with MaNGA ID 1-94604 and its control galaxies.
60SD
SS Im
age
1-94784 1-211063 1-135502
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
-0.67 -0.18 0.58
0.59 -0.01 -0.49
0.06 -0.11 0.23
-3.77 6.99 8.47
24.20 9.86 -12.92
11.03 9.01 6.31
22.68 72.50 74.30
-6.39 -22.10 39.78
15.12 75.45 61.28
-17.45 -91.47 -85.05
-22.02 -27.92 -104.51
-26.96 -101.90 -79.37
-0.06 -1.25 -1.28
-0.91 -1.46 -5.63
-0.62 -1.70 -1.72
Re = 6.5 kpc Re = 11 kpc Re = 12 kpc
A V (d
ex)
0.00.20.40.60.81.01.21.4
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A59. Comparison of the AGN with MaNGA ID 1-94784 and its control galaxies.
61SD
SS Im
age
1-95092 1-210962 1-251279
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.25 0.06 -0.04
-0.11 0.23 0.20
0.13 0.13 0.20
9.34 0.02 2.26
-2.53 0.34 4.71
4.42 0.07 5.16
41.95 61.83 26.68
-2.00 22.34 22.69
17.22 46.69 34.60
-54.64 -63.42 -32.24
-0.26 -28.06 -35.09
-24.99 -48.96 -44.75
-0.87 -0.59 -0.37
-0.09 -0.90 -0.53
-0.47 -0.64 -0.65
Re = 4.2 kpc Re = 8.7 kpc Re = 4.4 kpc
A V (d
ex)
0.0
0.2
0.4
0.6
0.8
1.0
1.2
0.0
0.1
0.2
0.3
0.4
0.5
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A60. Comparison of the AGN with MaNGA ID 1-95092 and its control galaxies.
62SD
SS Im
age
1-95585 1-166947 1-210593
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.15 0.37 -0.21
--- -1.04 0.30
0.15 0.39 0.04
17.35 6.71 0.21
--- 6.15 5.00
17.35 8.06 2.09
130.66 43.99 -1.35
--- -43.29 45.16
130.66 37.24 21.73
-175.82 -56.70 0.87
--- -53.74 -54.13
-175.82 -61.72 -25.92
-3.43 -1.18 -0.01
--- -8.50 -0.79
-3.43 -2.01 -0.37
Re = 32 kpc Re = 19 kpc Re = 6.8 kpc
A V (d
ex)
0.00.51.01.52.02.53.03.54.0
0.0
0.1
0.2
0.3
0.4
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A61. Comparison of the AGN with MaNGA ID 1-95585 and its control galaxies.
63SD
SS Im
age
1-96075 1-166947 1-52259
RGB
Map
s
AGN CTR1 CTR2AVxyxixo
< t>AVxyxixo
< t>AVxyxixo
< t>
0.0−
0.5 R e
0.5−
1.0 R e
0.0−
1.0 R e
0.03 0.37 -0.41
0.18 -1.04 0.20
0.31 0.39 -0.12
9.42 6.71 -2.73
16.19 6.15 19.30
16.68 8.06 7.12
58.88 43.99 10.61
20.26 -43.29 24.46
42.69 37.24 23.38
-73.45 -56.70 -10.03
-39.66 -53.74 -44.22
-61.79 -61.72 -31.05
-1.12 -1.18 -0.22
-1.28 -8.50 -1.80
-1.32 -2.01 -1.13
Re = 14 kpc Re = 19 kpc Re = 9.5 kpc
A V (d
ex)
0.00.51.01.52.02.53.03.54.0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
x yy +
xyo
(%)
0
10
20
30
40
50
x iy +
xii +
xio
(%)
0
20
40
60
80
100
x o (%
)
0
20
40
60
80
100
0
20
40
60
80
100
<t [l
og(y
r)]>
8.0
8.5
9.0
9.5
10.0
10.5
0.0 0.2 0.4 0.6 0.8 1.0RRe
8.0
8.5
9.0
9.5
10.0
10.5
11.0
Figure A62. Comparison of the AGN with MaNGA ID 1-96075 and its control galaxies.
