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<!-- DOI: 10.1051/0004-6361/200912540 -->

<h2 class="sec">Online Material</h2>
<A NAME="tab5"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/41/aa12540-09/table5.html"><span class="bold">Table 5:</span></a>&#160;&#160;
List of lines used in abundance determination using the Zeeman
spectrum.</p>
<p><A NAME="tab6"></A></p><p class="inset-old"><a href="/articles/aa/full_html/2009/41/aa12540-09/table6.html"><span class="bold">Table 6:</span></a>&#160;&#160;
List of lines used in abundance determination using the echelle
spectrum.</p>
<p></p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="lines"></A><!-- end Label--><A NAME="1268"></A><A NAME="figure1111" HREF="img158.png"><IMG SRC="Timg158.png" ALT="\begin{figure}
\par\includegraphics[width=18.5cm,clip]{12540f14.eps}
\end{figure}" HEIGHT="118" WIDTH="209"><!-- HTML Figure number: 14 --></td>
<td class="img-txt"><span class="bold">Figure 14:</span><p>
Section of the spectrum around sodium D1D2 lines. <i> From top
to bottom</i>: SAO&nbsp;echelle spectrum,
phase&nbsp;0.584, Rozhen Coud&#xe9; spectra, phases&nbsp;0.869
and&nbsp;0.291. Mesured radial velocities of primary&nbsp;(RVP)
and secondary (RVS) are marked. The synthetic spectrum of the secondary
is drawn with the proper radial velocity shift. The corresponding lines
in the primary and secondary component are outlined using arrows. Dots
above the echelle spectrum designate positions of telluric lines
contaminating the stellar spectrum, some of them are marked with
vertical bars. The spectra are shifted down by 0.2 in ordinate
intensity for clarity.</td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=14&DOI=10.1051/0004-6361/200912540" target="DEXTER">Open with DEXTER</a></td></tr>

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