  Recent results have shown that a substantial fraction of high-redshift Lyman
alpha galaxies contain considerable amounts of dust. This implies that Lyman
alpha galaxies are not primordial, as has been thought in the past. However,
this dust has not been directly detected in emission; rather it has been
inferred based on extinction estimates from rest-frame ultraviolet (UV) and
optical observations. This can be tricky, as both dust and old stars redden
galactic spectra at the wavelengths used to infer dust. Measuring dust emission
directly from these galaxies is thus a more accurate way to estimate the total
dust mass, giving us real physical information on the stellar populations and
interstellar medium (ISM) enrichment. New generation instruments such as the
Atacama Large Millimeter Array (ALMA) and Sub-Millimeter Array (SMA), should be
able to detect dust emission from some of these galaxies in the sub-mm. Using
measurements of the UV spectral slopes, we derive far-infrared flux predictions
for of a sample of 23 z > 4 Lyman alpha galaxies. We find that in only a few
hours, we can detect dust emission from 39 +/- 22% of our Lyman alpha galaxies.
Comparing these results to those found from a sample of 21 Lyman break galaxies
(LBGs), we find that LBGs are on average 60% more likely to be detected than
Lyman alpha galaxies, implying that they are more dusty, and thus indicating an
evolutionary difference between these objects. These observations will provide
better constraints on dust in these galaxies than those derived from their UV
and optical fluxes alone. Undeniable proof of dust in these galaxies could
explain the larger than expected Lyman alpha equivalent widths seen in many
Lyman alpha galaxies today.
