Using the results from a previously developed Ly \alpha /continuum production/transmission and dust enrichment model for Lyman Alpha Emitters ( LAEs ) , based on cosmological SPH simulations , we assess the detectability of their dust-reprocessed sub-millimeter ( submm ) radiation .
As supernovae ( rather than evolved stars ) control dust formation and destruction processes , LAEs are relatively dust-poor with respect to local galaxies : they have low dust-to-gas ratios ( 0.05 times the dust-to-gas ratio of the Milky Way ) in spite of their relatively high metallicity , Z \approx 0.1 - 0.5 Z _ { \odot } .
Using the derived escape fraction of ultraviolet ( UV ) continuum photons we compute the UV luminosity absorbed by dust and re-emitted in the far infrared .
The LAE submm fluxes correlate with their Ly \alpha luminosity : about ( 3 \%, 1 \% ) at z = ( 5.7 , 6.6 ) of the LAEs in our simulated sample ( those with with { Log } L _ { \alpha } > 43.1 ) would have fluxes at 850 \mu m ( the optimal band for detection ) in excess of 0.12 mJy and will be therefore detectable at 5 \sigma with ALMA with an integration time of only 1 hour .
Such detections would open a new window on the physical conditions prevailing in these most distant galaxies .