Modelling of Lyman-alpha Emitting Galaxies and Ionized Bubbles at the
  Era of Reionization
  Understanding Ly$\alpha$ emitting galaxies (LAEs) can be a key to reveal
cosmic reionization and galaxy formation in the early Universe. Based on halo
merger trees and Ly$\alpha$ radiation transfer calculations, we model redshift
evolution of LAEs and their observational properties at $z \ge 6$. We consider
ionized bubbles associated with individual LAEs and IGM transmission of
Ly$\alpha$ photons. We find that Ly$\alpha$ luminosity tightly correlates with
halo mass and stellar mass, while the relation with star formation rate has a
large dispersion. Comparing our models with the observed luminosity function by
Konno et al., we suggest that LAEs at $z \sim 7$ have galactic wind of $V_{\rm
out} \gtrsim 100~\rm km\, s^{-1}$ and HI column density of $N_{\rm HI} \gtrsim
10^{20}~\rm cm^{-2}$. Number density of bright LAEs rapidly decreases as
redshift increases, due to both lower star formation rate and smaller HII
bubbles. Our model predicts future wide deep surveys with next generation
telescopes, such as JWST, E-ELT and TMT, can detect LAEs at $z \sim 10$ with a
number density of $n_{\rm LAE} \sim {\rm a~few~} \times10^{-6} ~\rm Mpc^{-3}$
for the flux sensitivity of $10^{-18} ~\rm erg\, cm^{-2}\, s^{-1}$. By
combining these surveys with future 21-cm observations, it could be possible to
detect both LAEs with $L_{Ly\alpha} \gtrsim 10^{42}~\rm erg~s^{-1}$ and their
associated giant HII bubbles with the size $\gtrsim 250 ~\rm kpc$ at $z \sim
10$.
