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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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%           Extragalactic Astrophysics and Cosmology                         %
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\thematicarea{11}

\title{The Angular Clustering of WISE-selected AGN: Different Halos for
Obscured and Unobscured AGN}
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\author{Donoso E.\inst{1,2}, Yan L.\inst{3}, Stern D.\inst{4}, Assef R.J.\inst{4,5}}

\institute{Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET) \and
  Spitzer Science Center, California Institute of Technology, Pasadena, USA \and 
  Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, USA \and
  Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA \and
  Universidad Diego Portales, Santiago, Chile}

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\abstract{
We calculate the angular correlation function for a sample of $\sim$170,000 extracted
from the Wide-File Infrared Survey Explorer (WISE) catalog, selected to have red
mid-IR colors (W1-W2$>$0.8) and 4.6 $\mu$m flux densities brighter than 0.14 mJy.
The sample is expected to be >90\% reliable at identifying AGN, and to have a mean
redshift of $\langle z \rangle=1$. In total, the angular clustering of WISE AGN is
roughly similar to that of optical AGN. We cross-match these objects with the photometric
SDSS catalog and distinguish obscureds sources with r-W2$>$6 from bluer, unobscured AGN.
Obscured soruces present a higher angular clustering signal than unobscured sources.
Since the host galaxy morphologies of obscured AGN are not typical red sequence elliptical
galaxies and show disks in many cases, it is not likely that the increased clustering
strength of the obscured population is driven by a host galaxy segregation bias. By
using relatively complete redshift distributions from the COSMOS survey, we find obscured
sources at $\langle z \rangle=0.9$ have a bias of b=2.9$\pm$0.6 and are hosted in dark
matter halos with typical mass of log(M/M$\odot$ h$^{-1}$)$\sim$13.5. In contrast,
unobscured AGN at $\langle z \rangle=1.1$ have a bias of b=1.6$\pm$0.6 and inhabit halos
of log(M/M$\odot$ h$^{-1}$)$\sim$12.4. These findings suggest that unobscured AGN
inhabit denser environments than unobscured AGN, and are difficult to reconcile with
the simplest AGN unification models where obscuration is driven solely by orientation of
an obscuring dusty torus.}

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\keywords{Galaxies: active --- Galaxies: statistics --- Infrared: galaxies}

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\mail{edonoso@icate-conicet.gob.ar}

\maketitle

\end{document}
