Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[height=8cm,width=8.5cm,clip]{Hb021_f1.ps}\end{figure}$ Figure 1: Radial velocity measurements of HD 11977, taken with FEROS from October 1999 to November 2004. The measurements can be fitted with an orbital solution with a period of 711 days and an eccentricity of 0.4. The lower panel shows the residual velocity. The rms scatter of the residuals is partly due to intrinsic variability on short time scales, as commonly found for giant stars.
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In the text

$\begin{figure} \par\includegraphics[height=5.6cm,width=7cm,clip]{Hb021_f2.ps}\end{figure}$ Figure 2: The Lomb-Scargle periodogram of the radial velocity measurements. The periodogram shows a significant power at a frequency of 0.0014 cycles day^-1.
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In the text

$\begin{figure} \par\includegraphics[height=6cm,width=7.5cm,clip]{Hb021_f3a.ps}\par\includegraphics[height=6cm,width=7.5cm,clip]{Hb021_f3b.ps}\end{figure}$ Figure 3: The upper panel shows the region around the Ca II K emission lines. The relative flux K2V/K2R (lower panel) shows no long-period variation.
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In the text

$\begin{figure} \par\includegraphics[height=5.8cm,width=7.25cm,clip]{Hb021_f4.ps}\end{figure}$ Figure 4: Bisector velocity span (BVS) of HD 11977 calculated from the spectra taken between October 1999 and November 2004. The diagram shows no correlation between BVS and the measured radial velocities.
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In the text

$\begin{figure} \par\includegraphics[height=6.1cm,width=7.9cm,clip]{Hb021_f5.ps}\end{figure}$ Figure 5: Mass distribution of stars with known planetary companions (as of April 2005, including HD 11977). We exclude HD 13189 from this histogram due to the large uncertainty of the stellar mass.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.5cm,clip]{Hb021_f1.ps}\end{figure}$	Figure 1: Radial velocity measurements of HD 11977, taken with FEROS from October 1999 to November 2004. The measurements can be fitted with an orbital solution with a period of 711 days and an eccentricity of 0.4. The lower panel shows the residual velocity. The rms scatter of the residuals is partly due to intrinsic variability on short time scales, as commonly found for giant stars.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=5.6cm,width=7cm,clip]{Hb021_f2.ps}\end{figure}$	Figure 2: The Lomb-Scargle periodogram of the radial velocity measurements. The periodogram shows a significant power at a frequency of 0.0014 cycles day^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6cm,width=7.5cm,clip]{Hb021_f3a.ps}\par\includegraphics[height=6cm,width=7.5cm,clip]{Hb021_f3b.ps}\end{figure}$	Figure 3: The upper panel shows the region around the Ca II K emission lines. The relative flux K2V/K2R (lower panel) shows no long-period variation.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=5.8cm,width=7.25cm,clip]{Hb021_f4.ps}\end{figure}$	Figure 4: Bisector velocity span (BVS) of HD 11977 calculated from the spectra taken between October 1999 and November 2004. The diagram shows no correlation between BVS and the measured radial velocities.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=6.1cm,width=7.9cm,clip]{Hb021_f5.ps}\end{figure}$	Figure 5: Mass distribution of stars with known planetary companions (as of April 2005, including HD 11977). We exclude HD 13189 from this histogram due to the large uncertainty of the stellar mass.
Open with DEXTER