![\begin{figure}
\par\includegraphics[width=8cm,clip]{0922fig1.eps}
\end{figure}](/articles/aa/full/2004/37/aa0922/img47.gif) |
Figure 1: Part of the spectrum of HD 153720 . The axes are the wavelength in angstroms and relative flux. In the top part of the figure the points are the observed spectrum. The solid line is the sum of the synthetic spectra of the components. Scaled synthetic spectrum of the component A is shown separately in the middle part, of the component B - in the bottom part of the figure. Synthetic spectra of the components are shifted in accordance with the observed radial velocities and smoothed by instrumental and rotational profiles. The positions of the spectral lines, which were taken into account in synthetic spectra calculations are marked by short and long dashes (faint and strong lines). Some strong lines are identificated. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8cm,clip]{0922fig2.eps}
\end{figure}](/articles/aa/full/2004/37/aa0922/img48.gif) |
Figure 2:
The same as Fig. 1 in the vicinity of
the Ba II line  5853.688. The position
of this line in the spectrum of component B is marked
by a vertical broken line.
Three coadded synthetic spectra near the position of bariun lines
in component B correspond to the best barium abundance, and the
abundances changed by  0.5 dex with respect to the best abundance. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.3cm,clip]{0922fig3.eps}
\end{figure}](/articles/aa/full/2004/37/aa0922/img51.gif) |
Figure 3: The abundances of chemical elements in the atmosphere of HD 153720 A and B with respect to their abundances in the solar atmosphere. |
| Open with DEXTER | |
In the text