$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig4.eps} \end{figure}$ Figure 4: Synthetic spectrum fitting of Os II $\lambda$ 2067.229 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010C, R= 83 060, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.46, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0298fig5.eps} \end{figure}$ Figure 5: Synthetic spectrum fitting of Os II $\lambda$ 2070.693 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010C, R= 83 060, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.46, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig6.eps} \end{figure}$ Figure 6: Synthetic spectrum fitting of Os II $\lambda$ 2282.279 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010N, R= 90 620, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.14, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig7.eps} \end{figure}$ Figure 7: Synthetic spectrum fitting of Ir II $\lambda$ 2282.279 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010G, R= 84 585, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.28, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) iridium abundance.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig8.eps} \end{figure}$ Figure 8: The abundance pattern of ${\chi }$ Lupi A, relative to the solar system for the heaviest stable elements. A downward arrow represent an upper limit estimate.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0298fig1.eps} \end{figure}$	Figure 1: FTS recording of the a⁶D_7/2-z⁶F_9/2 Os II $\lambda$ 2067 transition.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0298fig2.eps} \end{figure}$	Figure 2: FTS recording of the a⁵F₄-z⁵D₃ Ir II $\lambda$ 2152 transition.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{0298fig3.eps} \end{figure}$	Figure 3: Comparison of log(gf) values from this work and data from Kurucz & Bell (1995).
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig4.eps} \end{figure}$	Figure 4: Synthetic spectrum fitting of Os II $\lambda$ 2067.229 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010C, R= 83 060, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.46, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0298fig5.eps} \end{figure}$	Figure 5: Synthetic spectrum fitting of Os II $\lambda$ 2070.693 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010C, R= 83 060, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.46, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig6.eps} \end{figure}$	Figure 6: Synthetic spectrum fitting of Os II $\lambda$ 2282.279 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010N, R= 90 620, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.14, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) osmium abundance.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{0298fig7.eps} \end{figure}$	Figure 7: Synthetic spectrum fitting of Ir II $\lambda$ 2282.279 in ${\chi }$ Lupi. The observed GHRS spectrum (Z16C010G, R= 84 585, $L_{{\rm pri}}$ / $L_{{\rm sec}}=$ 6.28, solid) is compared with synthetic spectra generated with the solar (dashed) and best-fit (dotted) iridium abundance.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0298fig8.eps} \end{figure}$	Figure 8: The abundance pattern of ${\chi }$ Lupi A, relative to the solar system for the heaviest stable elements. A downward arrow represent an upper limit estimate.
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