All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,height=7.4cm,clip]{0081fig1.ps} \end{figure}$ Figure 1: H-R diagram of the 83 giant stars in our RV survey with FEROS. The sample covers the RGB including the "clump'' region. The continuous lines are evolutionary tracks for solar-metallicity stars of masses comprised between 1.0 and 3.0 $M_{\hbox {$\odot $ }}$ , taken from Girardi et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,height=7.4cm,clip]{0081fig2.ps} \end{figure}$ Figure 2: RV plot of $\tau$ Cet (HD 10700) during the 2.5 years observation, the open circles represent the RV computation by the original method, the full filled circle are the final corrected RV. The final precision determined for FEROS during our survey is 22.8 ${\rm m~s}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,height=6.4cm,clip]{0081fig3.ps} \end{figure}$ Figure 3: Projected rotational velocity and rotational period. The - values in Table 1 (undetermined $v_{{\rm rot}}\sin{i}$ ) are not plotted.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=6.7cm,clip]{0081fig4.ps} \end{figure}$ Figure 4: Comparison of the stellar radii derived from the photometric determination and the values from the CHARM catalogue. The values are in an excellent agreement.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,height=9.7cm,clip]{0081fig5.ps} \end{figure}$ Figure 5: RV measurements of six binary systems: HD 7672, HD 27697, HD 40176, HD 62644, HD 156111 and HD 179799. The orbital parameters of the Kepler model and the mass-functions are given in Table 3.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.9cm,height=5.6cm,clip]{0081fig... ...m} \includegraphics[width=7.9cm,height=5.6cm,clip]{0081fig6b.ps} }\end{figure}$ Figure 6: Left: phase folded RV measurements of HD 7672. Right: the same for HD 156111 obtained from FEROS and TLS-Tautenburg.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{0081fig7a.ps}\hsp... ...cs[width=7.5cm,height=5.7cm,clip]{0081fig7c.ps}\hspace*{8.5cm} \par \end{figure}$ Figure 7: RV measurements of binary systems HD 21120, HD 22663, HD 176578, HD 187195 and HD 218527. These binaries show much longer period than our total observation span.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,height=7.4cm,clip]{0081fig8.ps} \end{figure}$ Figure 8: Color-magnitude diagram of the binaries found. The same evolutionary track as in Fig. 1 has been added. The primary masses can be estimated from the position in this diagram. The dots and triangles represent binaries with and without orbital solutions.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{0081fig9a.ps}\vspace*{5mm} \includegraphics[width=8cm,height=6cm,clip]{0081fig9b.ps} \end{figure}$ Figure 9: RV measurements of HD 27256 and HD 224533. These stars are known as stars in visual double systems. However, the measured RV variations are possibly due to other unseen companions.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,height=8.0cm,clip]{0081fig10.ps} \end{figure}$ Figure 10: Trend of RV variation - given by $\sigma _{{\overline {\rm RV}}}$ , listed in Table 4 - along the RGB. The scale of the dots gives the $\sigma _{{\overline {\rm RV}}}$ value. The $\sigma _{{\overline {\rm RV}}}$ in the upper part of the RGB is significantly larger than those in the lower and middle part as well as in the clump region. The cool luminous giant HD 151249 and the supergiant HD 78647 have the largest RV variabilities (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,height=5.8cm,clip]{0081fig11a.ps... ...mm} \includegraphics[width=7.7cm,height=5.8cm,clip]{0081fig11c.ps} \end{figure}$ Figure 11: 3 stars from different RGB regions are presented. HD 92588 - located in the lower of RGB - with $\sigma _{{\overline {\rm RV}}}$ less than 40 ${\rm m~s}^{-1}$ , HD 61935 represents stars in the middle of RGB with $\sigma _{\overline {\rm RV}}= 40$ -60 ${\rm m~s}^{-1}$ and HD 81797 on the upper part of RGB with $\sigma _{\overline {\rm RV}}> 60$ ${\rm m~s}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,height=7.6cm,clip]{0081fig12.ps} \end{figure}$ Figure 12: RV variability as a function of the stellar magnitude for the stars of our sample, after eliminating the stars with bona fide stellar companions. The two binaries with possible sub-stellar companions (HD 27256 and HD 224533) are given as dots, whereas stars hosting giant planet candidates HD 47536 and HD 122430 are indicated with filled triangles. Note the increase of spread and of minimum variability with increasing luminosity.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,height=7.4cm,clip]{0081fig13a.ps... ... \par\includegraphics[width=7.5cm,height=7.4cm,clip]{0081fig13b.ps} \end{figure}$ Figure 13: The upper panel shows the RV measurements of HD 78647. The lower panel presents the bisector velocity spans vs. the RV measurements. A clear correlation is present; together with variability detected in the Ca II K line, this indicates that the RV variability is induced by rotational modulation.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,height=7.4cm,clip]{0081fig1.ps} \end{figure}$	Figure 1: H-R diagram of the 83 giant stars in our RV survey with FEROS. The sample covers the RGB including the "clump'' region. The continuous lines are evolutionary tracks for solar-metallicity stars of masses comprised between 1.0 and 3.0 $M_{\hbox {$\odot $ }}$ , taken from Girardi et al. (2000).
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$\begin{figure} \par\includegraphics[width=8.0cm,height=7.4cm,clip]{0081fig2.ps} \end{figure}$	Figure 2: RV plot of $\tau$ Cet (HD 10700) during the 2.5 years observation, the open circles represent the RV computation by the original method, the full filled circle are the final corrected RV. The final precision determined for FEROS during our survey is 22.8 ${\rm m~s}^{-1}$ .
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$\begin{figure} \par\includegraphics[width=6.4cm,height=6.4cm,clip]{0081fig3.ps} \end{figure}$	Figure 3: Projected rotational velocity and rotational period. The - values in Table 1 (undetermined $v_{{\rm rot}}\sin{i}$ ) are not plotted.
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$\begin{figure} \par\includegraphics[width=6.8cm,height=6.7cm,clip]{0081fig4.ps} \end{figure}$	Figure 4: Comparison of the stellar radii derived from the photometric determination and the values from the CHARM catalogue. The values are in an excellent agreement.
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$\begin{figure} \par\includegraphics[width=15.4cm,height=9.7cm,clip]{0081fig5.ps} \end{figure}$	Figure 5: RV measurements of six binary systems: HD 7672, HD 27697, HD 40176, HD 62644, HD 156111 and HD 179799. The orbital parameters of the Kepler model and the mass-functions are given in Table 3.
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$\begin{figure} \par\mbox{\includegraphics[width=7.9cm,height=5.6cm,clip]{0081fig... ...m} \includegraphics[width=7.9cm,height=5.6cm,clip]{0081fig6b.ps} }\end{figure}$	Figure 6: Left: phase folded RV measurements of HD 7672. Right: the same for HD 156111 obtained from FEROS and TLS-Tautenburg.
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$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{0081fig7a.ps}\hsp... ...cs[width=7.5cm,height=5.7cm,clip]{0081fig7c.ps}\hspace*{8.5cm} \par \end{figure}$	Figure 7: RV measurements of binary systems HD 21120, HD 22663, HD 176578, HD 187195 and HD 218527. These binaries show much longer period than our total observation span.
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$\begin{figure} \par\includegraphics[width=7.6cm,height=7.4cm,clip]{0081fig8.ps} \end{figure}$	Figure 8: Color-magnitude diagram of the binaries found. The same evolutionary track as in Fig. 1 has been added. The primary masses can be estimated from the position in this diagram. The dots and triangles represent binaries with and without orbital solutions.
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$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{0081fig9a.ps}\vspace*{5mm} \includegraphics[width=8cm,height=6cm,clip]{0081fig9b.ps} \end{figure}$	Figure 9: RV measurements of HD 27256 and HD 224533. These stars are known as stars in visual double systems. However, the measured RV variations are possibly due to other unseen companions.
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$\begin{figure} \par\includegraphics[width=7.7cm,height=5.8cm,clip]{0081fig11a.ps... ...mm} \includegraphics[width=7.7cm,height=5.8cm,clip]{0081fig11c.ps} \end{figure}$	Figure 11: 3 stars from different RGB regions are presented. HD 92588 - located in the lower of RGB - with $\sigma _{{\overline {\rm RV}}}$ less than 40 ${\rm m~s}^{-1}$ , HD 61935 represents stars in the middle of RGB with $\sigma _{\overline {\rm RV}}= 40$ -60 ${\rm m~s}^{-1}$ and HD 81797 on the upper part of RGB with $\sigma _{\overline {\rm RV}}> 60$ ${\rm m~s}^{-1}$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,height=7.4cm,clip]{0081fig13a.ps... ... \par\includegraphics[width=7.5cm,height=7.4cm,clip]{0081fig13b.ps} \end{figure}$	Figure 13: The upper panel shows the RV measurements of HD 78647. The lower panel presents the bisector velocity spans vs. the RV measurements. A clear correlation is present; together with variability detected in the Ca II K line, this indicates that the RV variability is induced by rotational modulation.
Open with DEXTER