Online Material

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{figures/13750f4.ps} \end{figure}$	Figure 4: Comparison between the observed and theoretical profiles for the Ba 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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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{figures/13750f5.ps} \end{figure}$	Figure 5: Same as in Fig. 4 but for Ca.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{figures/13750f6.ps} \end{figure}$	Figure 6: Same as in Fig. 4 but for Si.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{figures/13750f7.ps} \end{figure}$	Figure 7: Same as in Fig. 4 but for Fe.
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$\begin{figure} \par\includegraphics[angle=90,width=15.5cm,clip]{figures/13750f9.ps} \end{figure}$

Figure 9:

Observed and theoretical energy distribution of HD 101065 calculated with scaled REE opacity from ISAN line list (see text). For comparison purpose the theoretical energy distribution of a normal F-type star HD 49933 is also shown. All theoretical calculations are smoothed with 20 Å Gaussian. Theoretical fluxes were scaled assuming radiuses: $R=1.98~R_\odot$ for HD 49933 and $T_{\rm eff}=6400$ K models; $R=1.90~R_{\odot}$ for $T_{\rm eff}=6500$ K; $R=1.82~R_{\odot}$ for $T_{\rm eff}=6600$ K.

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Table 3: List of Si, Ca, Fe, and Ba spectral lines used for reconstruction of chemical stratification.

Table 4: Abundances of individual elements.