All Figures

$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig1.ps} } \end{figure}$ Figure 1: Hipparcos light-curve phase-folded with the period from the light-curve of 0.435338 days. The primary eclipse is clearly visible, and the secondary eclipse is barely visible.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig2.ps} } \end{figure}$ Figure 2: Radial velocity measurements phase-folded with the period from the light-curve of 0.435338 days. The dashed line is for $f(m)={{M_2^3\sin^3{i}}\over{(M_1+M_2)^2}}=0.07~M_\odot$ . For the systems velocity the average RV of stars in the Tucana association of $20.6\pm 4.6$ is used km s^-1. Clearly, this curve does not fit the RV-measurements. BS Ind cannot be a simple eclipsing binary.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig3.ps} } \end{figure}$ Figure 3: The most likely orbital period is 3.3 years.
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In the text

$\begin{figure} \par {\includegraphics[width=6.7cm,clip]{2291fig4.ps} } \end{figure}$ Figure 4: A spectrum taken by Cutispoto et al. (2002) shows a double-peaked emission line structure in the Ca II K-line. In here we show as examples from top to bottom spectrum No. 4, No. 15, and No. 20. One emission core is seen but nothing obvious is seen from the companions.
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In the text

$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{2291fig5.ps} } \end{figure}$ Figure 5: CES spectrum of the FeI 6430.856 line of the K5V star $\rho$ Eri, and BS Ind. The spectral line of BS Ind is broader, because of the larger $v~\sin{i}$ but there is no obvious trace of the companions in this spectrum.
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In the text

$\begin{figure} \par {\includegraphics[width=6.7cm,clip]{2291fig6.ps} } \end{figure}$ Figure 6: The lower spectrum is the averaged of BS Ind. Averaged were all spectra from No. 10 to No. 19. since these have roughly the same RV. Above is a spectrum of an M0V star that is 2.9 mag fainter than BS Ind (shifted by 0.05). The TiO band-head at 7055 Å is the strongest feature in the spectrum of an M-dwarf. Even the averaged spectrum of BS Ind does not allow to exclude, or confirm the presence of such a companion.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{BS_Indi_min_max_ccM.ps} } \end{figure}$ Figure 7: Two cross-correlation functions. In both cases BS Ind is cross-correlated with an M0III-star. Apart from the sharp peak which is due to the primary KOV star, a broad feature is seen. This is the signature of the two eclipsing stars. Unfortunately the $v~\sin{i}$ of the tow eclsiping stars is so large that the two are not separated. Neverthless, we find that the broad peak changes its positions.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{BS_Indi-phaseII.ps} } \end{figure}$ Figure 8: The RV curve derived for the broad peak, after subtracting the 3.3 year orbit, and after phase-folding the data to the period of 0.435338 days. The filled dots are the phase averaged data points, and the open circles are the individual measurements. The phase is the same as in Fig. 1. The eclipse in fact appears, at $\rm RV=0$ , and before the primary eclipse the spectrum is red-shifted, just as it should be. Thus, there is clear evidence that the position of the broad peak varies with a period of 0.435338 days. The semi-amplitude is about 65 km s^-1.
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In the text

$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig1.ps} } \end{figure}$	Figure 1: Hipparcos light-curve phase-folded with the period from the light-curve of 0.435338 days. The primary eclipse is clearly visible, and the secondary eclipse is barely visible.
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$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig2.ps} } \end{figure}$	Figure 2: Radial velocity measurements phase-folded with the period from the light-curve of 0.435338 days. The dashed line is for $f(m)={{M_2^3\sin^3{i}}\over{(M_1+M_2)^2}}=0.07~M_\odot$ . For the systems velocity the average RV of stars in the Tucana association of $20.6\pm 4.6$ is used km s^-1. Clearly, this curve does not fit the RV-measurements. BS Ind cannot be a simple eclipsing binary.
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$\begin{figure} \par {\includegraphics[width=7cm,clip]{2291fig3.ps} } \end{figure}$	Figure 3: The most likely orbital period is 3.3 years.
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$\begin{figure} \par {\includegraphics[width=6.7cm,clip]{2291fig4.ps} } \end{figure}$	Figure 4: A spectrum taken by Cutispoto et al. (2002) shows a double-peaked emission line structure in the Ca II K-line. In here we show as examples from top to bottom spectrum No. 4, No. 15, and No. 20. One emission core is seen but nothing obvious is seen from the companions.
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$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{2291fig5.ps} } \end{figure}$	Figure 5: CES spectrum of the FeI 6430.856 line of the K5V star $\rho$ Eri, and BS Ind. The spectral line of BS Ind is broader, because of the larger $v~\sin{i}$ but there is no obvious trace of the companions in this spectrum.
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