$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f1.ps}\end{figure}$ Figure 1: Histogram of the standard deviations ( $\sigma$ ) of RV measurements for stars in the TLS sample. The $\sigma$ was computed after removing any obvious long term trends in the data that were due to stellar or substellar companions.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2850f2.ps}\end{figure}$ Figure 2: The spectral region of HD 13189 around 5170 Å ( bottom) compared to K-type stars of luminosity class I-V. The strong absorption features are the Mg I lines at 5167.3 Å, 5172.3 Å, and 5183.6 Å.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f3.ps}\end{figure}$ Figure 3: The radial velocity measurements for HD 13189 from TLS (circles), the Harlan J. Smith Telescope (HJS) of McDonald Observatory (triangles), and the Hobby-Eberly Telescope (HET, squares). The solid line represents the orbital solution.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f4.ps}\end{figure}$ Figure 4: Lomb-Scargle Periodogram of the RV measurements for HD 13189 for the TLS only data ( top panel), the TLS + HJS data ( bottom panel), and the combined data sets. The Lomb-Scargle (L-S) power is in arbitrary units that are a measure of the statistical significance of the peak.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f5.ps}\end{figure}$ Figure 5: The combined RV measurements for HD 13189 phased to the orbital period. The solid line is the orbital solution. Open circles represent repeated points plotted for the second cycle.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2850f6.ps}\end{figure}$ Figure 6: RV measurements of HD 13189 make on eight consecutive nights on the TLS 2 m telescope. The curve represents a least-squares sine fit with a period of 4.79 days and a full amplitude (K) of 168 m s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f7.ps}\end{figure}$ Figure 7: The Lomb-Scargle periodogram of the McDonald Ca II S-index measurements. The vertical line marks the orbital frequency.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f10.ps}\end{figure}$ Figure 10: Lomb-Scargle periodogram of the mean bisector span ( top) and curvature ( bottom) measurements. The vertical dashed line marks the location of the orbital frequency.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f11.ps}\end{figure}$ Figure 11: The phase-binned averages of the bisector span ( top) and curvature measurements ( bottom) phased to the orbital period.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{2850f12.ps}\end{figure}$ Figure 12: Lomb-Scargle Periodogram of the Hipparcos photometry for HD 13189. The vertical line marks the orbital frequency.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f1.ps}\end{figure}$	Figure 1: Histogram of the standard deviations ( $\sigma$ ) of RV measurements for stars in the TLS sample. The $\sigma$ was computed after removing any obvious long term trends in the data that were due to stellar or substellar companions.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2850f2.ps}\end{figure}$	Figure 2: The spectral region of HD 13189 around 5170 Å ( bottom) compared to K-type stars of luminosity class I-V. The strong absorption features are the Mg I lines at 5167.3 Å, 5172.3 Å, and 5183.6 Å.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f3.ps}\end{figure}$	Figure 3: The radial velocity measurements for HD 13189 from TLS (circles), the Harlan J. Smith Telescope (HJS) of McDonald Observatory (triangles), and the Hobby-Eberly Telescope (HET, squares). The solid line represents the orbital solution.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f4.ps}\end{figure}$	Figure 4: Lomb-Scargle Periodogram of the RV measurements for HD 13189 for the TLS only data ( top panel), the TLS + HJS data ( bottom panel), and the combined data sets. The Lomb-Scargle (L-S) power is in arbitrary units that are a measure of the statistical significance of the peak.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f5.ps}\end{figure}$	Figure 5: The combined RV measurements for HD 13189 phased to the orbital period. The solid line is the orbital solution. Open circles represent repeated points plotted for the second cycle.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2850f6.ps}\end{figure}$	Figure 6: RV measurements of HD 13189 make on eight consecutive nights on the TLS 2 m telescope. The curve represents a least-squares sine fit with a period of 4.79 days and a full amplitude (K) of 168 m s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f7.ps}\end{figure}$	Figure 7: The Lomb-Scargle periodogram of the McDonald Ca II S-index measurements. The vertical line marks the orbital frequency.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f8.ps}\end{figure}$	Figure 8: The McDonald S-index measurements phased to the orbital period.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f9.ps}\end{figure}$	Figure 9: The S-index measurements versus RV measurements from the McDonald data.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f10.ps}\end{figure}$	Figure 10: Lomb-Scargle periodogram of the mean bisector span ( top) and curvature ( bottom) measurements. The vertical dashed line marks the location of the orbital frequency.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2850f11.ps}\end{figure}$	Figure 11: The phase-binned averages of the bisector span ( top) and curvature measurements ( bottom) phased to the orbital period.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{2850f12.ps}\end{figure}$	Figure 12: Lomb-Scargle Periodogram of the Hipparcos photometry for HD 13189. The vertical line marks the orbital frequency.
Open with DEXTER