  We present a physically motivated semi-analytic model to understand the
clustering of high redshift Lyman Alpha Emitters (LAEs). We show that the model
parameters constrained by the observed luminosity functions, can be used to
predict large scale bias and angular correlation function of LAEs. These
predictions are shown to reproduce the observations remarkably well. We find
that average masses of dark matter halos hosting LAEs brighter than threshold
narrow band magnitude ~ 25 are ~ 10^11 M_\odot. These are smaller than that of
typical Lyman Break Galaxies (LBGs) brighter than similar threshold continuum
magnitude by a factor ~ 10. This results in a smaller clustering strength of
LAEs compared to LBGs. However, using the observed relationship between UV
continuum and Lyman-alpha luminosity of LAEs, we show that both LAEs and LBGs
belong to the same parent galaxy population with narrow band techniques having
greater efficiency in picking up galaxies with low UV luminosity. We also show
that the lack of evidence for the presence of the one halo term in the observed
LAE angular correlation functions can be attributed to sub-Poisson distribution
of LAEs in dark matter halos as a result of their low halo occupations.
