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<!-- DOI: 10.1051/0004-6361/200913750 -->

<h2 class="sec">Online Material</h2>
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<tr><td><!-- init Label --><A NAME="fig:pBa"></A><!-- end Label--><A NAME="1145"></A><A NAME="figure784" HREF="img46.png"><IMG SRC="Timg46.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{figures/13750f4.ps}
\end{figure}" HEIGHT="105" WIDTH="97"></A><!-- HTML Figure number: 7 -->
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<td class="img-txt"><span class="bold">Figure 4:</span><p>
Comparison between the observed and theoretical profiles for the
Ba&nbsp;lines. Observations are shown with symbols, thick full line
corresponds to the synthetic spectrum calculated with the best-fitting
stratified abundance distribution and dashed line shows prediction of
the spectrum synthesis with a homogeneous abundance.
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<tr><td><!-- init Label --><A NAME="fig:pCaIR"></A><!-- end Label--><A NAME="1146"></A><A NAME="figure789" HREF="img47.png"><IMG SRC="Timg47.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{figures/13750f5.ps}
\end{figure}" HEIGHT="52" WIDTH="98"></A><!-- HTML Figure number: 8 -->
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<td class="img-txt"><span class="bold">Figure 5:</span><p>
Same as in Fig.&nbsp;<a href="/articles/aa/full_html/2010/12/aa13750-09/aa13750-09.html#fig:pBa">4</a>
but for Ca.
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<tr><td><!-- init Label --><A NAME="fig:pSi"></A><!-- end Label--><A NAME="1147"></A><A NAME="figure795" HREF="img48.png"><IMG SRC="Timg48.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{figures/13750f6.ps}
\end{figure}" HEIGHT="102" WIDTH="97"></A><!-- HTML Figure number: 9 -->
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<td class="img-txt"><span class="bold">Figure 6:</span><p>
Same as in Fig.&nbsp;<a href="/articles/aa/full_html/2010/12/aa13750-09/aa13750-09.html#fig:pBa">4</a>
but for Si.
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<tr><td><!-- init Label --><A NAME="fig:pFe"></A><!-- end Label--><A NAME="1148"></A><A NAME="figure801" HREF="img49.png"><IMG SRC="Timg49.png" ALT="\begin{figure}
\par\includegraphics[width=8.8cm,clip]{figures/13750f7.ps}
\end{figure}" HEIGHT="106" WIDTH="97"></A><!-- HTML Figure number: 10 -->
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<td class="img-txt"><span class="bold">Figure 7:</span><p>
Same as in Fig.&nbsp;<a href="/articles/aa/full_html/2010/12/aa13750-09/aa13750-09.html#fig:pBa">4</a>
but for Fe.
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<tr><td><!-- init Label --><A NAME="fig:sed2"></A><!-- end Label--><A NAME="1149"></A><A NAME="figure809" HREF="img51.png"><IMG SRC="Timg51.png" ALT="\begin{figure}
\par\includegraphics[angle=90,width=15.5cm,clip]{figures/13750f9.ps}
\end{figure}" HEIGHT="67" WIDTH="175"></A><!-- HTML Figure number: 11 -->
</td>
<td class="img-txt"><span class="bold">Figure 9:</span><p>
Observed and theoretical energy distribution of HD&nbsp;101065
calculated with scaled REE&nbsp;opacity from ISAN&nbsp;line
list (see&nbsp;text). For&nbsp;comparison purpose the
theoretical energy distribution of a normal F-type star
HD&nbsp;49933 is also shown. All&nbsp;theoretical calculations
are smoothed with 20&nbsp;&#xc5;&nbsp;Gaussian. Theoretical fluxes
were scaled assuming radiuses:<!-- MATH: $R=1.98~R_\odot$ --> <IMG SRC="img50.png" ALT="$R=1.98~R_\odot$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="71">
for HD&nbsp;49933 and<!-- MATH: $T_{\rm eff}=6400$ --> <IMG SRC="img2.png" ALT="$T_{\rm eff}=6400$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="67">&nbsp;K
models;<!-- MATH: $R=1.90~R_{\odot}$ --> <IMG SRC="img33.png" ALT="$R=1.90~R_{\odot}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="72">
for<!-- MATH: $T_{\rm eff}=6500$ --> <IMG SRC="img6.png" ALT="$T_{\rm eff}=6500$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="67">&nbsp;K;
<!-- MATH: $R=1.82~R_{\odot}$ -->
<IMG SRC="img34.png" ALT="$R=1.82~R_{\odot}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="71">for&nbsp;
<!-- MATH: $T_{\rm eff}=6600$ -->
<IMG SRC="img8.png" ALT="$T_{\rm eff}=6600$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="67">&nbsp;K.
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<p><A NAME="tab:strat"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/12/aa13750-09/table3.html"><span class="bold">Table 3:</span></a>&#160;&#160;
List of Si, Ca, Fe, and Ba spectral lines used for reconstruction of
chemical stratification.</p>
<p><A NAME="tab:abn"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/12/aa13750-09/table4.html"><span class="bold">Table 4:</span></a>&#160;&#160;
Abundances of individual elements.</p>
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