  We performed an iron abundance determination of the hot, hydrogen deficient
post-AGB star PG1159-035, which is the prototype of the PG1159 spectral class
and the GW Vir pulsators, and of two related objects (PG1520+525, PG1144+005),
based on the first detection of Fe VIII lines in stellar photospheres. In
another PG1159 star, PG1424+535, we detect Fe VII lines. In all four stars,
each within Teff = 110,000 - 150,000 K, we find a solar iron abundance. This
result agrees with our recent abundance analysis of the hottest PG1159 stars
(Teff = 150,000 - 200,000 K) that exhibit Fe X lines. On the whole, we find
that the PG1159 stars are not significantly iron deficient, in contrast to
previous notions.
