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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{Modelo Anisótropo de Halos}

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\author{Sgró M.A.\inst{1}, Paz D.J.\inst{1,2}, Merchán M.E.\inst{1,2}}

\institute{Instituto de Astronomía Teórica y Experimental (CONICET-UNC) \and
  Observatorio Astron\'omico, Universidad Nacional de C\'ordoba}

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\abstract{El Modelo de Halos es una herramienta teórica que permite 
realizar predicciones sobre la distribución de materia en la estructura en 
gran escala del Universo (e.g., la función de correlación). En su forma estándar, 
estas predicciones son computadas asumiendo que los halos de materia oscura 
poseen forma perfectamente esférica y que no existen alineaciones preferenciales 
de la estructura circundante. Sin embargo, tanto las simulaciones numéricas como
los estudios realizados sobre grupos de galaxias, muestran que los halos poseen 
formas preferentemente proladas. Además, diversos trabajos han reportado
evidencias de alineamientos entre la forma de los halos y la distribución de materia
a su alrededor. 

En esta oportunidad, presentaremos una extensión del modelo de halos 
la cual considera la forma triaxial de los halos de materia oscura como así también 
incorpora un factor que controla las alineaciones observadas entre la forma de 
los halos y el material circundante. Dicho esquema, denominado {\it Modelo Anisótropo de 
Halos}, permite estimar las funciones de correlación anisótropas las cuales son 
definidas a lo largo de los semieje principales del tensor de forma de los halos.

Con el fin de caracterizar los alineamientos observados en simulaciones
numéricas y catálogos de grupos de galaxias, los resultados de nuestro modelo 
son contrastados con las funciones de correlación anisótropas obtenidas a partir 
de simulaciones numéricas y catálogos de galaxias.

Además de caracterizar las alineaciones de distribución de materia, este mejoramiento
del Modelo de Halos permitirá obtener mejores predicciones para otros campos
de la astronomía, tales como los estudios de lentes gravitacionales.
}

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\keywords{Cosmology: large-scale structure of universe --- 
          galaxies: halos --- 
          galaxies: groups: general --- 
					methods: statistical}

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\mail{marioagustin@oac.uncor.edu}

\maketitle

\end{document}
