All programme stars were classified in the framework of a refined MK system
described in Gray & Garrison (1987, 1989a,b). In addition we
used CP stars and confirmed 
Bootis stars
to guide us in the identification of peculiarities.
We classified the stars using the standard techniques of
MK classification although one of us (EP) used a simple mathematical
algorithm to help decide which standard star was closest to the programme
star under consideration. This was done by dividing the spectra into
several regions (e.g. H
, H
, CaIIK, etc.) and the standard
deviation with respect to a given MK standard
for each region was calculated resulting in a first estimation
(
2subclasses) of the spectral type.
For a precise classification of
the star as well as identification of possible peculiarities, the spectra
were compared visually with the MK standards using hardcopies (EP) or on the
computer graphics screen (ROG).
The most recent spectroscopic criteria for
membership in the Bootis group are given in Sect. 2.1 in Paunzen et
al. (1997) and Gray (1997).
Special care was taken in classifying high 
and probable
intermediate PopulationII stars (Gray 1988, 1989).
In Sect.6 (click here) all
confirmed and candidate Bootis stars are presented, results on "normal'' stars from
this sample
will be presented elsewhere (Paunzen & Heiter 1997).