  The velocity structure imprinted in the H{\alpha} emission line profiles
contains valuable information about galactic outflows. Using a set of
high-resolution zoom-in cosmological simulations of galaxies at z=2, we
generate H{\alpha} emission line profiles, taking into account the
temperature-dependent H{\alpha} emissivity, as well as dust extinction. The
H{\alpha} line can be described as a sum of two gaussians, as typically done
with observations. In general, its properties are in good agreement with those
observed in local isolated galaxies with similar masses and star formation
rates, assuming a spatially constant clumping factor of c=24. Blueshifted
outflows are very common in the sample. They extend several kpc above the
galaxy discs. They are also spread over the full extent of the discs. However,
at small radii, the material with high velocities tends to remain confined
within a thick disc, as part of galactic fountains or a turbulent medium, most
probably due to the deeper gravitational potential at the galaxy centre.
