@MastersThesis{DiazRamirez:2018:OrLiAl,
author = "Diaz Ramirez, Yaherlyn Elimar",
title = "Origem das linhas de alta ioniza{\c{c}}{\~a}o em n{\'u}cleos
ativos de Gal{\'a}xias",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2018",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2018-02-26",
keywords = "n{\'u}cleos gal{\'a}ticos ativos, linhas de alta
ioniza{\c{c}}{\~a}o, linhas coronais, fotoioniza{\c{c}}{\~a}o,
infravermelho: galaxias, active galaxy nuclei, high ionization
lines, coronal lines, fotoionization, infrared: galaxy.",
abstract = "N{\'u}cleos ativos de gal{\'a}xia (AGNs) apresentam em seus
espectros linhas proibidas de alta ioniza{\c{c}}{\~a}o ou linhas
coronais (CLs). Devido {\`a} energia necess{\'a}ria para sua
produ{\c{c}}{\~a}o (> 100 eV), as CLs tra{\c{c}}am uma parte
importante do cont{\'{\i}}nuo ionizante que nem sempre {\'e}
diretamente acess{\'{\i}}vel a partir de observa{\c{c}}{\~o}es
devido {\`a} absor{\c{c}}{\~a}o Gal{\'a}ctica e interna.
Sabe-se que as CLs s{\~a}o geralmente emitidas em regi{\~o}es
compactas pr{\'o}ximas {\`a} fonte central, mas as
condi{\c{c}}{\~o}es f{\'{\i}}sicas do g{\'a}s e os mecanismos
associados a sua produ{\c{c}}{\~a}o ainda est{\~a}o em debate.
Neste trabalho analisamos os parsecs mais internos de uma amostra
de 4 gal{\'a}xias ativas pr{\'o}ximas com emiss{\~a}o coronal
proeminente para estudar os mecanismos f{\'{\i}}sicos
respons{\'a}veis pela produ{\c{c}}{\~a}o das CLs. Com este
intuito, observa{\c{c}}{\~o}es de alta resolu{\c{c}}{\~a}o
angular ( 0.1/px) coletadas com espectr{\'o}grafos de campo
integral e {\'o}ptica adaptativa permitem estudar a
distribui{\c{c}}{\~a}o espacial do g{\'a}s de alta
ioniza{\c{c}}{\~a}o assim como modelar as raz{\~o}es [Si vi]/Br
, [S ix]/Pa, [Ca viii]/Br e [Si vii]/Br usando o c{\'o}digo de
fotoioniza{\c{c}}{\~a}o CLOUDY. Encontramos que a emiss{\~a}o
coronal nos objetos estudados {\'e} estendida, at{\'e}
dist{\^a}ncias da ordem de 150-200 pc. O g{\'a}s distribui-se
preferencialmente ao longo do jato r{\'a}dio em cada uma das
gal{\'a}xias. A distribui{\c{c}}{\~a}o do g{\'a}s {\'e}
altamente inhomog{\^e}nea, com m{\'u}ltiplos knots em
emiss{\~a}o. Mapas de canais mostram que a emiss{\~a}o coronal
{\'e} turbulenta, com velocidades de dispers{\~a}o acima dos 900
km s\−1. Modelos de fotoioniza{\c{c}}{\~a}o realizados
com CLOUDY comprovam que a fotoioniza{\c{c}}{\~a}o n{\~a}o
{\'e} o {\'u}nico mecanismo f{\'{\i}}sico respons{\'a}vel
pela emiss{\~a}o das linhas coronais. Processos energ{\'e}ticos
tais como choques s{\~a}o necess{\'a}rios para explicar a
emiss{\~a}o do g{\'a}s de alta ioniza{\c{c}}{\~a}o. De modo
geral, o nosso trabalho demonstra a utilidade de
observa{\c{c}}{\~o}es IFUs de alta resolu{\c{c}}{\~a}o angular
para entender, de forma mais acurada, os processos
f{\'{\i}}sicos nos parsecs mais internos dos AGNs. ABSTRACT:
Active galactic nuclei (AGNs) present, in their spectra, lines of
high ionization or coronal lines (CLs). Due to the potential
necessary for its production (> 100 eV), the CLs trace a part of
the ionizing continuum which is not always directly accessible
from observations due to Galactic and internal absorption. It is
known that CLs are generally emitted in compact regions near the
central source, but the physical conditions of the gas and the
mechanisms associated with their productio are under discussion.
In this work we analyze the most internal parsecs of a sample of 4
nearby active galaxies with prominent coronal emission to study
the physical mechanisms responsible for the production of CLs. For
this purpose, observations of high angular resolution ( 0.1/px)
collected with integral field spectroscopy and adaptive optics
allowed the study of the spatial distribution of the high
ionization gas and model the emission line flux ratios [Si vi]/Br
, [S ix]/Pa, [Ca viii]/Br and [Si vii]/Br using CLOUDY. We find
that the coronal emission in the studied objects is extended to
distances of up to 150-200 pc. The gas is distributed along the
radio jet in each of the galaxies. The gas distribution is highly
inhomogeneous, with multiple knots in emission. Channel maps show
that coronal emission is turbulent, with high velocity dispersion,
reaching values of 900 km s\−1. Photoionization models of
CLOUDY show that photoionization is not the only physical
mechanism responsible for the emission of coronal lines. Another
processes such as shocks are necessary to explain the emission of
the high ionization gas. Overall, our work highlights the need of
high angular IFU observations to understand, more accurately, the
physical processes associated to the central few parsecs in
AGNs.",
committee = "Rodrigues, Cl{\'a}udia Vilega (presidente) and Ardila, Alberto
Rodriguez (orientador) and Braga, Jo{\~a}o and Krabbe, Angela
Cristina",
englishtitle = "Origin of high ionization lines in active galactic nuclei",
language = "pt",
pages = "127",
ibi = "8JMKD3MGP3W34P/3QH9P4L",
url = "http://urlib.net/ibi/8JMKD3MGP3W34P/3QH9P4L",
targetfile = "publicacao real.pdf",
urlaccessdate = "28 mar. 2024"
}