  We present highlights and an overview of 20 FUSE and HST/STIS observations of
the bright symbiotic binary EG And. The main motivation behind this work is to
obtain spatially-resolved information on an evolved giant star in order to
understand the mass-loss processes at work in these objects. The system
consists of a low-luminosity white dwarf and a mass-losing, non-dusty M2 giant.
The ultraviolet observations follow the white dwarf continuum through periodic
gradual occultations by the wind and chromosphere of the giant, providing a
unique diagnosis of the circumstellar gas in absorption. Unocculted spectra
display high ionization features, such as the OVI resonance doublet which is
present as a variable (hourly time-scales), broad wind profile, which diagnose
the hot gas close to the dwarf component. Spectra observed at stages of partial
occultation display a host of low-ionization, narrow, absorption lines, with
transitions observed from lower energy levels up to ~5eV above ground. This
absorption is due to chromospheric/wind material, with most lines due to
transitions of SiII, PII, NI, FeII and NiII, as well as heavily damped HI Lyman
series features. No molecular features are observed in the wind acceleration
region despite the sensitivity of FUSE to molecular hydrogen. From analysis of
the ultraviolet dataset, as well as optical data, we find that the dwarf
radiation does not dominate the wind acceleration region of the giant, and that
observed thermal and dynamic wind properties are most likely representative of
isolated red giants.
