- 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
- 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.