The original computer code (Sahal-Bréchot 1969a,b), has been modernized, updated and optimized several times (Sahal-Bréchot 1974; Fleurier et al. 1977; Dimitrijevic & Sahal-Bréchot 1984; Dimitrijevic et al. 1991; Dimitrijevic & Sahal-Bréchot 1996b). A summary of the formalism is given in Dimitrijevic & Sahal-Bréchot (1996b), and will not be repeated here. Atomic energy levels needed for calculations have been taken from Martin et al. (1990). Oscillator strengths have been calculated within the Coulomb approximation (Bates & Damgaard 1949, and the tables of Oertel & Shomo 1968). For higher levels, the method of Van Regemorter et al. (1979) has been used.
Our results for 34 S V
multiplets
are shown in Table 1 (accessible only in electronic form), for
perturber densities 
and temperatures 
. The complete
set of data is given for the
perturber density of 
. For
perturber density of 
, only data for higher
transitions, needed for better
interpolation with perturber density are given. Stark broadening
parameters for densities lover than tabulated, are
linear with perturber density.
We also
specify a parameter c (Dimitrijevic & Sahal-Bréchot 1984),
which gives an estimate for the maximum perturber density for which
the line may be treated
as isolated when it is divided by the
corresponding full width at half maximum. For
each value given in Table 1, the collision
volume (V) multiplied by the perturber density (N) is much
less than one and the impact approximation is valid
(Sahal-Bréchot 1969a,b). Values for NV > 0.5 are not given
and values for 
are denoted by an asterisk.
When the impact approximation is not valid, the ion
broadening contribution may be estimated by using
quasistatic approach (Sahal-Bréchot 1991 or Griem
1974). In the region between where neither of these two
approximations is valid, a unified type theory should be used. For example
in Barnard et al. (1974), a simple analytical formulas for such
a case are given. The accuracy of the results obtained decreases when
broadening by ion interactions becomes important.
We hope that presented results will be useful for the interpretation and modelling of sdO stars spectra as well as for subphotospheric layers research and for laboratory plasma considerations. For further development and rafinement of the Stark broadening theory for multicharged ion lineshapes, as well as for the investigation of regularities and systematic trends of Stark broadening parameters along isoelectronic sequences, the corresponding experimental data will be very useful.
Acknowledgements
This work is a part of the project "Astrometrical, Astrodynamical and Astrophysical Investigations", supported by Ministry of Science and Technology of Serbia.