HAWAII     SCUBA     IMAGING

Seeing Galaxy Formation in a Cold Light

THE  FUTURE


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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