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At this time the key task is to refine the 850µ counts
through additional very deep field imaging and wider-field shallow
surveys. This is likely to take place in the coming year through
the combined efforts of the Hawaii, UK and Canadian groups working
on this problem. The next key piece of information we need is
a determination of the redshift distribution of the sources,
and while this can be estimated from optical or submillimeter
color constraints, ulitmately it must be done spectroscopically
to be convincing. It is likely that this will be easiest for the
lensed sample of Smail et al. and hopefully we will see parallel
progress on this using the LRIS spectrograph on the KeckII 10m
telescope, and spectrographs on the 4m class telescopes. Finally
we will need to obtain improved constraints on the bolometric
corrections to fully understand the submillimeter star formation
history. Some progress on this may be possible by determining
the relation between 175µ sources seen with the ISOPHOT
instrument on the ISO mission (Kawara et al., Lagache et al.) and
the 850µ source population, but it is possible that this
aspect of the problem may not be fully solved until future
space missions are flown.
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