All Figures

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{4208fg1.ps}\end{figure}$ Figure 1: The amplitude spectrum of the radial velocity variations for 10 telluric lines. The standard deviation in amplitude is formally only 1 m s^-1 from a least squares fit to the data, but we estimate from this diagram that $\sigma = 2$ m s^-1 is more realistic.
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4208fg2a.ps}\vspace*{3mm} \includegraphics[width=5.9cm,clip]{4208fg2b.ps}\end{figure}$ Figure 2: The top panel shows the amplitude spectrum of the radial velocity variations for the Fe I 6165.36 Å line. The bottom panel shows the amplitude spectrum for six Fe I lines. Both panels are for night 1 when the magnetic phase was 0.09.
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4208fg3a.ps}\par\includegraphics[width=5.9cm,clip]{4208fg3b.ps}\end{figure}$ Figure 3: The top panel shows the amplitude spectrum of the radial velocity variations for the Ce II 6272.026 Å line. The bottom panel shows the amplitude spectrum for four Ce II lines. Both panels are for night 1 when the magnetic phase was 0.09.
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4208fg4a.ps}\vspace*{3mm} ... ...g4b.ps}\vspace*{3mm} \includegraphics[width=5.9cm,clip]{4208fg4c.ps}\end{figure}$ Figure 4: The top panel shows the amplitude spectrum of the radial velocity variations for the Nd III 6550.330 Å line on our first night. This line often shows high radial velocity amplitude in other roAp stars, so it caught our attention. The middle panel shows the amplitude spectrum the Nd II 5319.815 Å line on our second night. This line also often shows high radial velocity amplitude in other roAp stars, so again the peak in intriguing, but it cannot be confirmed for our first night, as is shown in the bottom panel. Neither of the peaks in the top two panels can be found in any other line either, so they are spurious.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{4208fg1.ps}\end{figure}$	Figure 1: The amplitude spectrum of the radial velocity variations for 10 telluric lines. The standard deviation in amplitude is formally only 1 m s^-1 from a least squares fit to the data, but we estimate from this diagram that $\sigma = 2$ m s^-1 is more realistic.
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$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4208fg2a.ps}\vspace*{3mm} \includegraphics[width=5.9cm,clip]{4208fg2b.ps}\end{figure}$	Figure 2: The top panel shows the amplitude spectrum of the radial velocity variations for the Fe I 6165.36 Å line. The bottom panel shows the amplitude spectrum for six Fe I lines. Both panels are for night 1 when the magnetic phase was 0.09.
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$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4208fg3a.ps}\par\includegraphics[width=5.9cm,clip]{4208fg3b.ps}\end{figure}$	Figure 3: The top panel shows the amplitude spectrum of the radial velocity variations for the Ce II 6272.026 Å line. The bottom panel shows the amplitude spectrum for four Ce II lines. Both panels are for night 1 when the magnetic phase was 0.09.
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