All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{9169fig1.ps} \end{figure}$ Figure 1: C, N, and F yields from AGB models of different masses and [Fe/H] = -2.3. Note that the F yields are plotted on a different scale.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{9169fig2.ps} \end{figure}$ Figure 2: Abundances by number of F and C+N with respect to H as observed in HE 1305+0132 with 1 $\sigma$ errors, taken from Schuler et al. (2007, hatched ellipsoid), and computed in the average material lost via the winds by AGB stars at [Fe/H] = -2.3, with labels indicating the initial masses. The initial composition is scaled from solar. The gray area is the region of the plot where the F and C+N abundances from the AGB companion should lie to ensure that the observed abundances are reproduced after dilution. The darker gray area represents the region covered by our models with masses in the range indicated by the asterisks.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{9169fig1.ps} \end{figure}$	Figure 1: C, N, and F yields from AGB models of different masses and [Fe/H] = -2.3. Note that the F yields are plotted on a different scale.
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