All Figures

$\begin{figure} \par\includegraphics[height=6.15cm,width=6cm,clip]{3852fig1.eps}\end{figure}$ Figure 1: Experimental device.
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In the text

$\begin{figure} \par\includegraphics[height=4.1cm,width=5.4cm,clip]{3852fig2.eps}\end{figure}$ Figure 2: A typical Os II experimental decay curve with an exponential fit. The lifetime for this level, situated at 39 389.49 cm^-1, is 66(6) ns.
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In the text

$\begin{figure} \par\includegraphics[height=4cm,width=5.3cm,clip]{3852fig3.eps}\end{figure}$ Figure 3: Detected time-resolved fluorescence signal from the level at 46 776.29 cm^-1 in Os I and the recorded excitation laser pulse. The convolution procedure gives a lifetime of 4.8 (0.3) ns.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3852fig4.eps}\end{figure}$ Figure 4: Comparison between experimental and theoretical even energy levels in Os II. The calculations have been performed with 3 scaling factors (SF = 0.80, 0.85 and 0.90).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3852fig5.eps}\end{figure}$ Figure 5: Same as Fig. 4 for odd levels of Os II.
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In the text

$\begin{figure} \par\includegraphics[height=14cm,width=7.4cm,clip]{3852fig6.eps}\end{figure}$ Figure 6: Osmium lines at 326.7945, 330.1559 and 442.0468 nm (as indicated by the dotted vertical lines). The thick dotted line is the observed solar spectrum, and the 3 thin lines correspond (from top to bottom in each subfigure) to spectral synthesis (i) with no osmium; (ii) with the Os abundance as listed in Table 8; and (iii) with the former standard solar Os abundance $\log \varepsilon_{\rm Os}$ = 1.45. These spectral synthesis have been produced with the MARCS solar model taking the isotopic and hyperfine structures into account.
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In the text

$\begin{figure} \par\includegraphics[height=4.25cm,width=6.7cm,clip]{3852fig7.ps}\end{figure}$ Figure 7: The Os I 330.1559 nm line in a carbon-rich metal-poor star. The thick line corresponds to the observed spectrum of the CH star HD 187861. The thin lines correspond to spectral synthesis using a dedicated MARCS model without osmium, and with an osmium abundance of $\log \varepsilon_{\rm Os}$ = 0.55.
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In the text

$\begin{figure} \par\includegraphics[height=6.15cm,width=6cm,clip]{3852fig1.eps}\end{figure}$	Figure 1: Experimental device.
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$\begin{figure} \par\includegraphics[height=4.1cm,width=5.4cm,clip]{3852fig2.eps}\end{figure}$	Figure 2: A typical Os II experimental decay curve with an exponential fit. The lifetime for this level, situated at 39 389.49 cm^-1, is 66(6) ns.
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$\begin{figure} \par\includegraphics[height=4cm,width=5.3cm,clip]{3852fig3.eps}\end{figure}$	Figure 3: Detected time-resolved fluorescence signal from the level at 46 776.29 cm^-1 in Os I and the recorded excitation laser pulse. The convolution procedure gives a lifetime of 4.8 (0.3) ns.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3852fig4.eps}\end{figure}$	Figure 4: Comparison between experimental and theoretical even energy levels in Os II. The calculations have been performed with 3 scaling factors (SF = 0.80, 0.85 and 0.90).
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3852fig5.eps}\end{figure}$	Figure 5: Same as Fig. 4 for odd levels of Os II.
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$\begin{figure} \par\includegraphics[height=4.25cm,width=6.7cm,clip]{3852fig7.ps}\end{figure}$	Figure 7: The Os I 330.1559 nm line in a carbon-rich metal-poor star. The thick line corresponds to the observed spectrum of the CH star HD 187861. The thin lines correspond to spectral synthesis using a dedicated MARCS model without osmium, and with an osmium abundance of $\log \varepsilon_{\rm Os}$ = 0.55.
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