All Figures

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig1.eps} \end{figure}$ Figure 1: The observed spectrum of HD 221170 (squares) and the synthetic spectra (solid lines) calculated with our final abundances. The axes are the wavelength in angstroms and relative fluxes. The positions of the spectral lines taken into account in the calculations are marked in the bottom part of the figure by short and long dashes. For some of the strong lines, the identification and isotopic composition for molecular lines are given. The position of the Hf II 4093.155 Å line is marked by a vertical dotted line. The different synthetic spectra correspond to a Hf abundance lower or higher by 0.5 dex with respect to the abundance obtained from the optimum value.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig2.eps} \end{figure}$ Figure 2: Same as Fig. 1 in the vicinity of the Pb I 4057.806 Å line. The three different synthetic spectra correspond to the optimum lead abundance and a deviation by $\pm$ 0.5 dex from this value. Note that the unmarked strong line on the blueside of the Pb line corresponds to the ¹²CH line. The separation of the ¹²CH and Pb lines is smaller thanthe instrumental profile, so that the uncertainties in the determination of the wavelength and oscillator strength can strongly affect the Pb abundance determination.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig3.eps} \end{figure}$ Figure 3: Same as Fig. 1 in the vicinity of the Th II 4019.129 Å line. The different synthetic spectra correspond to the mean thorium abundance of -1.18 (in the scale log N(H) = 12) and a deviation by $\pm$ 0.5 dex from this value.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig4.eps} \end{figure}$ Figure 4: Same as Fig. 3 in the vicinity of the Th II 4094.747 Å line.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig5.eps} \end{figure}$ Figure 5: Same as Fig. 3 in the vicinity of the Th II 5989.045 Å line.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig6.eps} \end{figure}$ Figure 6: Same as Fig. 1 in the vicinity of the U II 4050.041 Å line. The different synthetic spectra correspond to a uranium abundance of -2.52, -2.02, and -1.72 (in the scale log N(H) = 12).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1540fig7.eps} \end{figure}$ Figure 7: The abundances of chemical elements and ions in the atmosphere of HD 221170 with respect to the solar atmosphere value. Triangles correspond to upper limits for Li, Al, U.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig8.eps} \end{figure}$ Figure 8: Comparison of the surface abundances in HD 221170 with the solar system r-abundance distribution scaled to the observed Er abundance. The solar system abundances corresponds to the photospheric determination of Grevesse & Sauval (1998) with the solar r-process distribution estimated by Goriely (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig3.eps} \end{figure}$	Figure 3: Same as Fig. 1 in the vicinity of the Th II 4019.129 Å line. The different synthetic spectra correspond to the mean thorium abundance of -1.18 (in the scale log N(H) = 12) and a deviation by $\pm$ 0.5 dex from this value.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig4.eps} \end{figure}$	Figure 4: Same as Fig. 3 in the vicinity of the Th II 4094.747 Å line.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig5.eps} \end{figure}$	Figure 5: Same as Fig. 3 in the vicinity of the Th II 5989.045 Å line.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig6.eps} \end{figure}$	Figure 6: Same as Fig. 1 in the vicinity of the U II 4050.041 Å line. The different synthetic spectra correspond to a uranium abundance of -2.52, -2.02, and -1.72 (in the scale log N(H) = 12).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1540fig7.eps} \end{figure}$	Figure 7: The abundances of chemical elements and ions in the atmosphere of HD 221170 with respect to the solar atmosphere value. Triangles correspond to upper limits for Li, Al, U.
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$\begin{figure} \par\includegraphics[width=8.25cm,clip]{1540fig8.eps} \end{figure}$	Figure 8: Comparison of the surface abundances in HD 221170 with the solar system r-abundance distribution scaled to the observed Er abundance. The solar system abundances corresponds to the photospheric determination of Grevesse & Sauval (1998) with the solar r-process distribution estimated by Goriely (1999).
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