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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{ms3557.f1} \end{figure}$ Figure 1: The region near the core of the CaII K line for the Sun ( $\log R^{'}_{HK}=-4.94$ ), the components of HD 219542 and the active star 36 Oph A ( $\log R^{'}_{HK}=-4.58$ , Henry et al. 1996). The spectra for the other stars were arbitrarily shifted in intensity with respect to the solar one. The horizontal lines represent the zero level for each spectrum. The vertical lines show the spectral region used for chromospheric activity measurement (the continuum regions are outside the plotted range).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{ms3557.f2} \end{figure}$ Figure 2: The calibration of R^'_HK index based on 11 stars with literature determinations, observed with the FEROS spectrograph during our observing run (August 2002) and instrument commissioning (Kaufer et al. 1999).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{ms3557.f3} \end{figure}$ Figure 3: Galactic orbit of HD 219542 in the meridional plane.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{ms3557.f4} \end{figure}$ Figure 4: Lithium determinations for Hyades stars from Thorburn et al. (1993) (empty circles for abundance measurements and empty triangles for upper limits) and for the components of HD 219542 (HD 219542 A: filled circle; HD 219542 B: filled triangle). Only an upper limit was derived for HD 219542 B. The line at the lower left corner represents variations of derived lithium content as a function of the adopted effective temperature. Even assuming large differences in the temperature scales used by Thorburn et al. (1993) and Paper I of $\sim$ 150-200 K, it is not possible to obtain a lithium content for HD 219542 similar to that of the stars of Hyades of similar temperature.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3557.f5} \end{figure}$ Figure 5: Astrometric measurements of HD 219542. Overplotted is the best linear fit to the data.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3557.f6} \end{figure}$ Figure 6: Possible values of semimajor axis, period, eccentricity and periastron distance of the orbit of HD 219542 as a function of the (unknown) separation along the line of sight.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3557.f7} \end{figure}$ Figure 7: Critical semiaxis for dynamical stability of planets orbiting HD 219542 A (upper panel) and HD 219542 B (lower panel) as a function of the current separation along the line of sight.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f8} \end{figure}$ Figure 8: Differential radial velocities of HD 219542 A. The dispersion of the velocities is 5.8 m s^-1, compatible with measurement errors.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f9} \end{figure}$ Figure 9: Differential radial velocities of HD 219542 B. Overplotted is the best Keplerian solution.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f10} \end{figure}$ Figure 10: Residuals of the velocities of HD 219542 B from the calculated orbit.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f11} \end{figure}$ Figure 11: The velocities of HD 219542 B phased to the 112.1 days period of the best orbital solution.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{ms3557.f12} \end{figure}$ Figure 12: Lomb-Scargle periodogram results for the RV data of component A (upper panel) and component B (lower panel). The false-alarm-probability (FAP) levels of $1\%$ are indicated as horizontal dashed lines (see text for details). While there is no signal present for HD 219542 A, we find a strong peak at P=111 days for HD 219542 B. However, even this signal has a FAP of $3.7\%$ and is thus not highly significant.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{ms3557.f13} \end{figure}$ Figure 13: Left panel: Cross Correlation Function for a spectrum of HD 219542 B; right panel: superposition of the the mean line bisectors from the spectra of 51 Peg (dotted line), HD 219542 A (dashed line), and HD 219542 B (solid line). T and B regions are those used in the computation of the bisector span.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3557.f14} \end{figure}$ Figure 14: Bisector span measurements vs. radial velocities for HD 219542 B (upper panel) and HD 219542 A (lower panel). There are not significant correlations for both stars. On the right corner the typical short term error on bisector span measurement is shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{ms3557.f15} \end{figure}$ Figure 15: Limits on planets around HD 219542 A in circular (dashed line) and eccentric (continuous line) orbits derived using the Monte Carlo procedure described in the text.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{ms3557.f16} \end{figure}$ Figure 16: Limits on planets around HD 219542 B in circular (dashed line) and eccentric (continuous line) orbits derived using the Monte Carlo procedure described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{ms3557.f2} \end{figure}$	Figure 2: The calibration of R^'_HK index based on 11 stars with literature determinations, observed with the FEROS spectrograph during our observing run (August 2002) and instrument commissioning (Kaufer et al. 1999).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{ms3557.f3} \end{figure}$	Figure 3: Galactic orbit of HD 219542 in the meridional plane.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3557.f5} \end{figure}$	Figure 5: Astrometric measurements of HD 219542. Overplotted is the best linear fit to the data.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{ms3557.f6} \end{figure}$	Figure 6: Possible values of semimajor axis, period, eccentricity and periastron distance of the orbit of HD 219542 as a function of the (unknown) separation along the line of sight.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{ms3557.f7} \end{figure}$	Figure 7: Critical semiaxis for dynamical stability of planets orbiting HD 219542 A (upper panel) and HD 219542 B (lower panel) as a function of the current separation along the line of sight.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f8} \end{figure}$	Figure 8: Differential radial velocities of HD 219542 A. The dispersion of the velocities is 5.8 m s^-1, compatible with measurement errors.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f9} \end{figure}$	Figure 9: Differential radial velocities of HD 219542 B. Overplotted is the best Keplerian solution.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f10} \end{figure}$	Figure 10: Residuals of the velocities of HD 219542 B from the calculated orbit.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{ms3557.f11} \end{figure}$	Figure 11: The velocities of HD 219542 B phased to the 112.1 days period of the best orbital solution.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{ms3557.f13} \end{figure}$	Figure 13: Left panel: Cross Correlation Function for a spectrum of HD 219542 B; right panel: superposition of the the mean line bisectors from the spectra of 51 Peg (dotted line), HD 219542 A (dashed line), and HD 219542 B (solid line). T and B regions are those used in the computation of the bisector span.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3557.f14} \end{figure}$	Figure 14: Bisector span measurements vs. radial velocities for HD 219542 B (upper panel) and HD 219542 A (lower panel). There are not significant correlations for both stars. On the right corner the typical short term error on bisector span measurement is shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{ms3557.f15} \end{figure}$	Figure 15: Limits on planets around HD 219542 A in circular (dashed line) and eccentric (continuous line) orbits derived using the Monte Carlo procedure described in the text.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{ms3557.f16} \end{figure}$	Figure 16: Limits on planets around HD 219542 B in circular (dashed line) and eccentric (continuous line) orbits derived using the Monte Carlo procedure described in the text.
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