All Figures

$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig1.eps} \end{figure}$ Figure 1: Line profile fit for PG 1219+534 using solar metalicity models (top panel) and metal-rich models (10 times solar, bottom panels). The Balmer lines and He II at 4686 Å match simultaneously when using the metal rich models (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=8.1cm,clip]{3948fig2.eps} \end{figure}$ Figure 2: Same as Fig. 1 but for CD $-24^\circ 731$ .
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=8.4cm,clip]{3948fig3.eps} \end{figure}$ Figure 3: Comparison of a 15 Å wide section of the near- and far-UV spectrum of PG 1219+534. In the NUV it is possible to measure the continuum level, while in the FUV it must be estimated. Note also the higher flux in the FUV.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3948fig4.eps} \end{figure}$ Figure 4: Spectrum fit to the C III multiplet at 1174-1177 Å for Feige 48. The model is shown as the thick line. Other strong lines due to Cr IV and Fe IV are marked.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig5.eps} \end{figure}$ Figure 5: The S III resonance lines for CPD $-64^\circ 481$ , showing an excellent match. The line at $\sim$ 1194.5 Å is one of the Si II resonance lines, while the strong line at $\sim$ 1194.15 Å is unidentified.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=8cm,clip]{3948fig6.eps} \end{figure}$ Figure 6: A region of spectrum showing blended iron-group lines for Feige 48, PG 1219+534 and Feige 66. The line at $\sim$ 1858.2 Å is unidentified.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig7a.eps}\p... ...e*{3mm} \includegraphics[angle=360,width=7.8cm,clip]{3948fig7b.eps} \end{figure}$ Figure 7: Determination of microturbulent velocity of CD $-24^\circ 731$ and PG 1219+534 using Cr III lines. We find $\xi =5^{+2}_{-1}$ km s^-1 for the former, while the latter is consistent with $\xi =0$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3948fig8.eps} \end{figure}$ Figure 8: Spectrum fit to the C IV resonance lines at 1550 Å for Feige 66. The model is shown as the thick line. The line cores of the model do not match the observations, and the abundance is set around 0.8 dex lower than that derived from C III lines. See text for details.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=15.5cm,clip]{3948fig9.eps} \end{figure}$ Figure 9: Abundances measured for our five targets. Magenta symbols represent values determined using singly ionised lines, green represents doubly ionised lines, red represents triply ionised lines, blue denotes quadruply ionised lines and cyan represents upper limits. Note the generally excellent agreement between different ionisation stages.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3948fig10.eps} \end{figure}$ Figure 10: Spectrum fit to the Ge IV resonance lines at 1189 Å for Feige 66. The model is shown as the thick line.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=7.1cm,clip]{3948fig11.eps} \end{figure}$ Figure 11: Trends in heavy element abundances with iron abundance.
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=8cm,clip]{3948fig12.eps} \end{figure}$ Figure 12: Comparison of iron-group abundances for our pulsator/non-pulsator pairs (F48 = Feige 48; CPD = CPD $-64^\circ 481$ ; PG = PG 1219+534; CD = CD $-24^\circ 731$ ; F66 = Feige 66). The dotted lines denote equal abundances and the difference in iron abundance. The differences between PG 1219+534, CD $-24^\circ 731$ and Feige 66 are quite large - particularly for Fe, Ni and Mn - while the pairs PG 1219+534 and CD $-24^\circ 731$ and Feige 48 and CPD $-64^\circ 481$ show quite similar abundances, in particular when the differences in iron abundance are accounted for (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig1.eps} \end{figure}$	Figure 1: Line profile fit for PG 1219+534 using solar metalicity models (top panel) and metal-rich models (10 times solar, bottom panels). The Balmer lines and He II at 4686 Å match simultaneously when using the metal rich models (see text).
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$\begin{figure} \par\includegraphics[angle=360,width=8.1cm,clip]{3948fig2.eps} \end{figure}$	Figure 2: Same as Fig. 1 but for CD $-24^\circ 731$ .
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$\begin{figure} \par\includegraphics[angle=360,width=8.4cm,clip]{3948fig3.eps} \end{figure}$	Figure 3: Comparison of a 15 Å wide section of the near- and far-UV spectrum of PG 1219+534. In the NUV it is possible to measure the continuum level, while in the FUV it must be estimated. Note also the higher flux in the FUV.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3948fig4.eps} \end{figure}$	Figure 4: Spectrum fit to the C III multiplet at 1174-1177 Å for Feige 48. The model is shown as the thick line. Other strong lines due to Cr IV and Fe IV are marked.
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$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig5.eps} \end{figure}$	Figure 5: The S III resonance lines for CPD $-64^\circ 481$ , showing an excellent match. The line at $\sim$ 1194.5 Å is one of the Si II resonance lines, while the strong line at $\sim$ 1194.15 Å is unidentified.
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$\begin{figure} \par\includegraphics[angle=360,width=8cm,clip]{3948fig6.eps} \end{figure}$	Figure 6: A region of spectrum showing blended iron-group lines for Feige 48, PG 1219+534 and Feige 66. The line at $\sim$ 1858.2 Å is unidentified.
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$\begin{figure} \par\includegraphics[angle=360,width=7.8cm,clip]{3948fig7a.eps}\p... ...e*{3mm} \includegraphics[angle=360,width=7.8cm,clip]{3948fig7b.eps} \end{figure}$	Figure 7: Determination of microturbulent velocity of CD $-24^\circ 731$ and PG 1219+534 using Cr III lines. We find $\xi =5^{+2}_{-1}$ km s^-1 for the former, while the latter is consistent with $\xi =0$ km s^-1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3948fig8.eps} \end{figure}$	Figure 8: Spectrum fit to the C IV resonance lines at 1550 Å for Feige 66. The model is shown as the thick line. The line cores of the model do not match the observations, and the abundance is set around 0.8 dex lower than that derived from C III lines. See text for details.
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$\begin{figure} \par\includegraphics[angle=360,width=15.5cm,clip]{3948fig9.eps} \end{figure}$	Figure 9: Abundances measured for our five targets. Magenta symbols represent values determined using singly ionised lines, green represents doubly ionised lines, red represents triply ionised lines, blue denotes quadruply ionised lines and cyan represents upper limits. Note the generally excellent agreement between different ionisation stages.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3948fig10.eps} \end{figure}$	Figure 10: Spectrum fit to the Ge IV resonance lines at 1189 Å for Feige 66. The model is shown as the thick line.
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$\begin{figure} \par\includegraphics[angle=360,width=7.1cm,clip]{3948fig11.eps} \end{figure}$	Figure 11: Trends in heavy element abundances with iron abundance.
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