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We perform Monte-Carlo radiative transfer calculations to model the Lymanalpha properties of galaxies in high-resolution, zoom-in cosmologicalsimulations at z ~ 6.6. The simulations include both constrained andunconstrained runs, representing respectively a highly overdense region and anaverage field. Different galactic wind models are used in the simulations inorder to investigate the effects of these winds on the apparent Ly alphaproperties of galaxies. We find that, for models including galactic winds, theLy alpha properties of massive galaxies residing in the overdense region matchwell recent observations of luminous Ly alpha emitters (LAEs) at z ~ 6-7, interms of apparent Ly alpha luminosity, Ly alpha line width and Ly alphaequivalent width distributions. Without winds, the same galaxies appear less Lyalpha bright as a result of both differences in the line profile emerging fromgalaxies themselves, and, in the distributions of neutral gas in thecircumgalactic (CGM) and intergalactic medium (IGM). We also study therelations between apparent Ly alpha luminosity and various galaxy properties:stellar mass, star formation rate (SFR) and host halo mass. At fixed halo mass,the apparent Ly alpha luminosity of galaxies appears to depend on thelarge-scale environment while this is no longer true for galaxies at a givenstellar mass or SFR. We provide simple linear fits to these relations that canbe used for quickly constructing mock LAE samples from N-body simulations. Ourresults suggest that the observed luminous LAEs at z ~ 6.6 are hosted by~10^{12} h^{-1} Mo, dark matter haloes, residing in large, overdense ionizedregions.

Lyman alpha Properties of Simulated Galaxies in Overdense Regions: Effects of Galactic Winds at z > 6