  PG1159 stars are hot hydrogen-deficient post-AGB stars with effective
temperatures within a range from 75000 K up to 200000 K. These stars are
probably the result of a late helium-shell flash that had occurred during their
first descent from the AGB. The lack of hydrogen is caused by flash-induced
envelope mixing and burning of H in deeper regions. Now the former intershell
matter is seen on the surface of the stars. Hence the stellar atmospheres show
metal abundances drastically different from the solar values. Our sample
comprises ten PG1159 stars with effective temperatures between 85000 K and
170000 K. We present first results of our spectral analysis based on FUV
spectra obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE).
