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\documentclass[craaa]{aaa2014}

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\usepackage[spanish,activeacute,english]{babel}
\usepackage[utf8]{inputenc}
\usepackage{verbatim}
\usepackage{amsmath}
\usepackage{amsfonts}
\usepackage{amssymb}

\begin{document}

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\journalvol{57}
\journalyear{2014}
\journaleditors{A.C. Rovero, C. Beaugé, L.J. Pellizza, M. Lares}

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\contribtype{2}

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%  11 [AEC]: Astrofísica Extragaláctica y Cosmología /                       %
%           Extragalactic Astrophysics and Cosmology                         %
%  12 [EG]: Estructura Galáctica / Galactic Structure                        %
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\thematicarea{11}

\title{An\'alisis espectral en rayos-X de galaxias Seyfert 1.}

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\author{M.\ V.\ Cardaci\inst{1,2}, G.\ F.\ H\"agele\inst{1,2}}

\institute{Instituto de Astrof\'isica de La Plata (IALP-CONICET-UNLP) \and
  Facultad de Ciencias Astron\'omicas y Geof\'isicas de La Plata (UNLP)}

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\abstract{
Las galaxias Seyfert son una de las clases m\'as comunes
de n\'ucleos activos de galaxias (AGN: Active Galactic Nucleus), son menos luminosas que los cu\'asares, pero suelen estar mejor estudiadas
porque su proximidad las hace m\'as brillantes en todas las frecuencias. 
Son d\'ebiles en radio y sus espectros \'opticos muestran l\'ineas de
emisi\'on indicativas de la existencia de gas ionizado que se 
mueve con velocidades de al menos 1000km/s y que puede alcanzar hasta decenas
de miles de km/s en las galaxias Seyfert y cu\'asares de tipo 1.
El modelo m\'as aceptado para los n\'ucleos activos es que la causa \'ultima
de su potencia es la liberaci\'on de energ\'ia gravitatoria en el proceso de
acreci\'on de materia hacia un agujero negro supermasivo (10$^{6}$-10$^9$\,M$_\odot$). Seg\'un el modelo est\'andar las diferencias 
entre unos y otros tipos son debidas a la existencia de material denso en sus
proximidades, con una distribuci\'on asim\'etrica 
que oculta la parte central del n\'ucleo activo cuando es observado con
determinadas orientaciones. 
En este esquema, en las galaxias Seyfert 1 este material no intercepta nuestra
l\'inea de visi\'on y podemos ver incluso las partes m\'as internas. Sin
embargo, al ser objetos extragal\'acticos, y 
tener tama\~nos muy peque\~nos, no podemos resolver su estructura con las
t\'ecnicas de observaci\'on 
disponibles. Necesitamos inferir sus propiedades a trav\'es de estudios
espectrales y de variabilidad. 
El an\'alisis espectral en rayos-X de las principales
caracter\'isticas de los AGNs ha revelado
gran parte de la naturaleza de los procesos f\'isicos en las regiones
internas de estos objetos. La imagen que ha surgido para explicar lo
observado en el rango de energ\'ias 1.5 -- 15 keV (o incluso hasta 200 keV) a
partir del an\'alisis de la informaci\'on colectada por la actual generaci\'on
de telescopios de rayos-X (XMM-Newton y Chandra) contiene, como primera
aproximaci\'on, unos pocos ingredientes: un plasma caliente emisor en rayos-X
y un material fr\'io irradiado, y la mayor parte de las observaciones en
rayos-X blandos requiere la inclusi\'on de gas ionizado absorbente/emisor en
la l\'inea de la visi\'on. 
El estudio de las caracter\'isticas espectrales observadas
en la banda de rayos-X en las galaxias Seyfert 1 dista mucho de ser
homog\'eneo. Dicha homogeneidad es necesaria para encarar un an\'alisis
comparativo e intentar interpretar los resultados en t\'erminos de la
evoluci\'on, formaci\'on estelar asociada, tipo de galaxia hu\'esped y
condiciones f\'isicas y din\'amicas de este tipo de objetos.
En este trabajo presentamos un breve resumen de los resultados que hemos
obtenido aplicando una misma metodolog\'ia de an\'alisis a los datos de
algunas galaxias Seyfert 1 obtenidos con el sat\'elite XMM-Newton, y algunos
de nuestros proyectos en v\'ias de desarrollo.
}

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\keywords{galaxies: active --- galaxies: Seyfert --- galaxies: general --- X-rays: galaxies}


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\mail{mcardaci@fcaglp.unlp.edu.ar}

\maketitle

\end{document}
