Spectra of the bright symbiotic star AG Draconis ( BD+67 ^ { \circ } 922 ) in the wavelength range 905–1187 Å 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 Å 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 \lambda 1032 are identified at wavelengths 1141.172 Å and 1142.429 Å , 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 \lambda 997/ \lambda 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 2 s ^ { 2 } 2 p ^ { 2 } ^ { 3 } P _ { 0 , 1 } – 2 s 2 p ^ { 3 } ^ { 5 } S _ { 2 } and Ne vi 2 s ^ { 2 } 2 p ^ { 2 } P _ { J } – 2 s 2 p ^ { 2 } ^ { 4 } P _ { J ^ { \prime } } 
transitions are published .