Clustering and lifetime of Lyman Alpha Emitters in the Epoch of
  Reionization
  We calculate Lyman Alpha Emitter (LAE) angular correlation functions (ACFs)
at $z \simeq 6.6$ and the fraction of lifetime (for the 100 Myrs preceding
$z\simeq6.6$) galaxies spend as Lyman Break Galaxies (LBGs) or as LBGs with
Lyman Alpha (Ly$\alpha$) emission using a model that combines SPH cosmological
simulations (GADGET-2), dust attenuation and a radiative transfer code
(pCRASH). The ACFs are a powerful tool that significantly narrows the 3D
parameter space allowed by LAE Ly$\alpha$ and UV luminosity functions (LFs)
alone. With this work, we simultaneously constrain the escape fraction of
ionizing photons $f_{esc}=0.05-0.5$, the mean fraction of neutral hydrogen in
the intergalactic medium (IGM) $\langle \chi_{HI} \rangle \leq 0.01$ and the
dust-dependent ratio of the escape fractions of Ly$\alpha$ and UV continuum
photons $f_{\alpha}/f_c=0.6-1.2$. Our results show that reionization has the
largest impact on the amplitude of the ACFs, and its imprints are clearly
distinguishable from those of $f_{esc}$ and $f_\alpha/f_c$. We also show that
galaxies with a critical stellar mass of $M_* = 10^{8.5} (10^{9.5})M_{\odot}$
produce enough luminosity to stay visible as LBGs (LAEs). Finally, the fraction
of time during the past 100 Myrs prior to z=6.6 a galaxy spends as a LBG or as
a LBG with Ly$\alpha$ emission increases with the UV magnitude (and the stellar
mass $M_*$): considering observed (dust and IGM attenuated) luminosities, the
fraction of time a galaxy spends as a LBG (LAE) increases from 65% to 100%
(0-100%) as $M_{UV}$ decreases from $M_{UV} = -18.0$ to $-23.5$ ($M_*$
increases from $10^8-10^{10.5} M_{\odot}$). Thus in our model the brightest
(most massive) LBGs most often show Ly$\alpha$ emission.
