  We explore the relationship between the spectral shape of the Ly{\alpha}
emission and the UV morphology of the host galaxy using a sample of 304
Ly{\alpha}-emitting BV i-dropouts at 3 < z < 7 in the GOODS and COSMOS fields.
Using our extensive reservoir of high-quality Keck DEIMOS spectra combined with
HST WFC3 data, we measure the Ly{\alpha} line asymmetries for individual
galaxies and compare them to axial ratios measured from observed J- and H-band
(restframe UV) images. We find that the Ly{\alpha} skewness exhibits a large
scatter at small elongation (a/b < 2), and this scatter decreases as axial
ratio increases. Comparison of this trend to radiative transfer models and
various results from literature suggests that these high-redshift Ly{\alpha}
emitters are not likely to be intrinsically round and symmetric disks, but they
probably host galactic outflows traced by Ly{\alpha} emitting clouds. The
ionizing sources are centrally located, with the optical depth a good indicator
of the absorption and scattering events on the escape path of Ly{\alpha}
photons from the source. Our results find no evidence for evolution in
Ly{\alpha} asymmetry or axial ratio with look-back time.
