High resolution spectra of the program stars were
obtained with the 6 m and 1 m Telescopes of the Special
Astrophysical Observatory during 1993-94. The Nasmyth
echelle spectrometer LYNX (Panchuk et al. 1993) and
coude-echelle spectrometer CEGS (Musaev 1993, 1996)
equipped with the 
pixels CCD detector
were used. The LYNX service observations were carried out
by the 6-m telescope staff Drs. G. Galazutdinov, V.G.
Klochkova, and V.E. Panchuk in the time intervals
allocated to L. Zacs by the 6-m Telescope Programmes
Committee. The program stars were selected with the aim
to define a sample of binary systems with orbital
parameters similar to those of barium stars but for a
range of orbital periods (P), mass function (f(M)),
and eccentricity (e) values to provide an optimal
condition to analyze the sufficient conditions for the
formation of the chemical peculiarities. Some binary
systems with F-G dwarfs as primaries were included in the
observation program since it is supposed that mass
transfer can occur also to the main sequence star. In
addition two mild (Ba 1.0) BaII stars with a constant
radial velocity (RV) were selected (Jorissen 1994) to
check the enhancement of the heavy elements. 
(G8IIIab) was chosen as a primary comparison standard
of chemical composition and Procyon (F5IV-V) was used as
a secondary standard to establish the properties of
dwarfs. About thirty single line spectroscopic binaries
were selected for this program mainly from the eighth
catalogue of Batten et al. (1989). Table 1 (click here) gives the
physical data for 19 stars and two standards discussed in
this work. The spectral classification were taken from
Hoffleit (1982) and Yamashita & Norimoto (1981).
Apparent magnitudes are from Hoffleit (1982). The sixth
column indicates the telescope used for observations. The
orbital elements of spectroscopic binaries were taken
from Batten et al. (1989).
Table 1: Physical data and observations mode for the program stars. Last three
columns indicate orbital period, eccentricity, and mass function, respectively
The LYNX spectra covered the spectral region 
in 30
wavelength bands (overlapping in regions from 5000 to 5200 Å). Each region
spanned from 50 to 80 Å and had a signal-to-noise ratio in the range of
70-150. The resolution, as measured from the FWHM of lines from a thorium lamp,
was 30 000 (
at 5500 Å). The CEGS spectra
covered the spectral region from 4400 Å to 6900 Å. The 39
wavelength regions were observed at a resolution of 
depending on the wavelength. Each region spanned 
. Most of these spectra have a S/N more than 100. LYNX and
CEGS wavelengths regions in the red (
)
spectral region are similar.
The raw spectra were reduced for CCD dark current, echelle-grating
scattered light, cosmic particle events, divided by flat-fields and
wavelength calibrated using standard DECH routines realized in SAO
on IBM PC (Galazutdinov 1992). The continuum of the red giant
spectrum was defined by a number of narrow spectral regions,
selected to be relatively free of lines. The sample of spectra from
the program stars are shown in Figs. 1 (click here) and 2 (click here) along with those of
standards 
and Procyon. Figures 1 (click here) and 2 (click here) show spectra
near the BaII lines 6141.72 Å and 6496.90 Å used for the
determination of Ba abundance. The 6587 Å CI line region is
illustrated in Fig. 3 (click here). The lines for the abundance analysis were
chosen to be as free as possible of blends. Lines showing no
significant line asymmetry were measured by interactively fitting
Gaussian functions to the line profiles. The number of lines
measured per star was typically 500-700, however, as a rule the
lines stronger than 200 mÅ were not used in the analyses. The
internal accuracy of the equivalent widths is of order 5% based on
comparison of values obtained from overlapping spectra. The list of
lines used in the abundance analysis and measured equivalent widths
for each star will be published separately. The external accuracy
of the equivalent widths can be assessed by comparing our results
with independent measurements of common stars by other authors.
Equivalent widths for a few of the program stars are available from
the published analyses. In Figs. 4 (click here)a and b a comparison for standard
stars is shown. As can be seen the equivalent widths scales are in
general consistent.
Figure 1: Sample spectra for 
and 
along with the
standard Procyon in the wavelength range 
. Measured features
include BaII 6141.72 Å, FeII 6149.24 Å, NaI 6154.22 Å, OI 6155.99 Å,
6156.78 Å, 6158.19 Å, CaI 6162.17 Å, and FeI 6180.21 Å
Figure 2: Sample spectra for HD 160538 and HD 119185 along with the standard
in the wavelength range 
. Measured
features include NiI 6482.81 Å, CaI 6493.78 Å, BaII 6496.9 Å, FeII 6516.05
Å, and LaII 6526.95 Å