Following our successful survey of the Northern Hubble Deep Field
at 6.7 and 15 mu, we propose to survey the Southern Hubble Deep
with CAM at the same wavelengths.
Data reduction on the Northern HDF is nearing completion and we hope
to release the data received to date in November.  We believe that
we have detected a number of HDF galaxies both at 6.7 and 15 mu
We have been carrying out a detailed study of the Hubble Deep Field (HDF) since
its release and have published a paper on the nature of the faint galaxies
detected in the HDF (Mobasher et al 1996).  The key point for ISO
is the very high proportion of very blue, star-forming galaxies in the
sample.  80% of the galaxies have colours consistent with being in the process
of undergoing vigorous star formation and it is a reasonable expectation that
a high proportion of them will have strong far infrared excesses.
We have used our standard starburst spectral energy distributions (Pearson and
Rowan-Robinson 1996, MN in press) to predict the 6.7 and 15 mu fluxes from the
HDF galaxies.  We predict that the most sensitive CAM detectors (LW2 and LW3)
are capable of detecting tens of HDF galaxies with S/N=5 in integrations of
2 hours per detector for each of the 3 WF fields.  This is close to the conf-
usion limit for CAM, so that longer integrations are unlikely to be worthwhile.
The software we are already developing for analysis of the ELAIS data has been
adapted for analysis of the HDF fields and we have a strong team
to carry out this data analysis at ICSTM, supported by the other teams of the
consortium.  Our expertise in the analysis of ISO survey data, coupled with the
detailed work we have been carrying out on the HDF, ensures that high-quality
data and science analysis products would be delivered to the community if
this proposal were successful.