  We investigate the sources and amount of dust in early galaxies. We discuss
dust nucleation in stellar atmospheres using published extended atmosphere
models, stellar evolution tracks and nucleation conditions and conclude that
the (TPAGB) phase of intermediate mass stars is likely to be the most promising
site for dust formation in stellar winds. The implications of chemical
evolution models for high redshift galaxies are investigated and we show there
is no difficulty in producing dusty galaxies at redshifts above 5 if supernovae
are a dominant source of interstellar dust. If dust does not condense
efficiently in SNe then significant dust masses can only be generated at by
galaxies with a high star formation efficiency. We find the visual optical
depth for individual star forming clouds can reach values greater than 1 at
very low metallicity (1/100 solar) provided that the mass-radius exponent of
molecular clouds is less than two. Most of the radiation from star formation
will emerge at IR wavelengths in the early universe provided that dust is
present. The (patchy) visual optical depth through a typical early galaxy will
however, remain less than 1 on average until a metallicity of 1/10 solar is
reached.
