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%  This template defines the format for the submission of contributions      %
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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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\contriblanguage{0}

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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                        %
%  13 [AE]: Astrofísica Estelar / Stellar Astrophysics                       %
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\thematicarea{11}

\title{El Impacto de la Reionización en las Historias de Formación Estelar de las Galaxias Enanas.}

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\author{Alejandro Benítez-Llambay\inst{1}, Mario G. Abadi\inst{1}}

\institute{Instituto de Astronomía Teórica y Experimental (IATE), Laprida 854, X5000BGR, Córdoba, Argentina}

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\abstract{Las galaxias enanas cercanas muestran una gran diversidad en sus historias de formación estelar: desde sistemas viejos que completaron su formación estelar 10 mil millones de años atrás hasta sistemas jóvenes, que formaron la mayor parte de sus estrellas en los últimos 5 mil millones de años o sistemas en los cuales coexisten una cantidad similar de estrellas jóvenes y viejas. Sin embargo, cuando todos estos sistemas son considerados en conjunto, se observa que exhiben una marcada disminución en su formación estelar en tiempos intermedios (entre $4 \le t \le 8$ mil millones de años).

Utilizando simulaciones cosmológicas hidrodinámicas de la formación del Grupo Local de Galaxias, hemos identificado a la reionización del Universo (la cual habría ocurrido entre $6 \le z_{reion} \le 10$) como la principal responsable de la baja eficiencia de formación estelar en tiempos intermedios. A saber, la reionización del Universo a alto redshift calienta el gas, el cual es removido de los halos de baja masa, afectando típicamente halos cuya temperatura virial es menor que $\sim 2 \times 10^4 K$. La pérdida de bariones induce una disminución en la actividad de formación estelar, la cual, ayudada por el feedback de la formación estelar temprana, vacía de gas a los halos y produce sistemas caracterizados por una única población estelar vieja. En halos cuya temperatura virial en $z_{reion}$ es menor que el límite anterior, el calentamiento debido a la reionización induce un retraso en la formación estelar hasta que el halo se hace más masivo y permite que parte del gas restante se enfríe y forme estrellas. De esta manera, una única población jóven domina en halos que colapsan más tarde. Sistemas caracterizados por dos componentes estelares (una vieja y una jóven) son el resultado de fusiones tardías entre los dos ejemplos anteriores. Así, la disminución en la eficiencia de la formación estelar de las galaxias enanas cercanas sería la característica más clara ya observada del impacto que la reionización ha tenido en su formación. }




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\keywords{galaxies: dwarf  --- galaxies: formation --- Cosmology: dark ages, reionization, first stars}

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\mail{alejandrobll@oac.uncor.edu}

\maketitle

\end{document}
