Our proposal is to observe 8 symbiotic stars with the SWS.  In 5 of
these cases, the data will be used to determine the line contribution
to 5 to 60 micron broad band photometry taken with PHT-P within the GT
programme NOVAE.  This will allow an accurate estimate of the cool dust
continuum variation with wavelength, enabling us to fit the distribution
with an emissivity weighted black-body, and derive physical parameters
such as temperature and dust grain crystallinity (from the beta index).
In addition we will be able to identify the lines which are clearly
influencing the PHT-P results, and so draw conclusions about the
abundances and chemistry of the emitting regions.  In the 3 remaining
cases, we are concentrating on lines already detected in SWS01
observations.  Observations of the 10 micron silicate profile in each
star will allow us to determine the degree of crystallinity or
amorphousness of the silicate grains. High-resolution scans of a
number of unidentified lines (thought to be Ne, O, and H recombination)
will enable an unambigous identification using the profile shapes and
line ratios, and provide information on the velocity distribution of
the emitting gas.