Astronomy & Astrophysics

Table 1: Atmospheric parameters of the program stars as taken from the literature. The neon abundance has been set to 2%. Abundances are given in % mass fraction.
Table 2: Log of FUSE and VLT observations of our program stars. VLT observations were performed with two different instrumentalsetups (see text).
Table 3: Ne VII lines identified in UV (vacuum wavelengths) and optical (air wavelength) spectra of PG 1159 stars. The last column gives the excitation energy of the lower level of the line transition. Level energies for the 3853-3912 Å multiplet are from Kelly (1987), but line positions determined from our observations. As a consequence, the uncertainty in Kelly's energy for the lower level is $x\protect\la1600$ cm^-1.
Table 4: Summary of Ne VII line identifications in our program stars. "+'' and "-'' denote detection and non-detection, respectively. "broad'' means that the detected line is much broader than the computed one. No entry means that no spectra are available. The second column denotes if the star is a pulsator (+) or non-pulsator (-). No entry means, that no photometric observations were performed or published.