  Spectra of the bright symbiotic star AG Draconis (BD+67D922) in the
wavelength range 905-1187 A obtained with the Far Ultraviolet Spectroscopic
Explorer (FUSE) are presented. The spectra show a number of narrow, nebular
emission lines, together with a uniform continuum from the hot component of the
system, and numerous interstellar absorption lines. We infer the existence of
Ne VIII in the AG Dra nebula through the identification of the Ne VII 973.3 A
recombination line. The emission line spectrum is dominated by intense lines of
O VI, but also shows weaker lines from highly-ionized ions including Ne V, Ne
VI, S IV, S VI. Members of the He II Balmer series can be identified up to
n=20. Lines of Fe II and Fe III fluoresced by O VI 1032 are identified at
wavelengths 1141.172 A and 1142.429 A, respectively. The emission lines are
shown to be produced in a plasma with an electron temperature of 20-30,000 K,
photoionized by the white dwarf. The Ne VI 997/999 ratio shows that this ion
and all others except perhaps Ne VII are formed at least 300 white dwarf radii
from the white dwarf. Revised wavelengths for the Ne V 2s^2 2p^2 ^3P_0,1 - 2s
2p^3 ^5S_2 and Ne VI 2s^2 2p ^2P_J - 2s 2p^2 ^4P_J' transitions are published.
