All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{5756fg1.eps} \end{figure}$ Figure 1: Proper-motion vector point diagram in the area of IC 2391. A clump of proper motions at $\mu _x=-20.1$ and $\mu _y=+17.6$ mas yr^-1indicates the location of the cluster.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{5756fg2.eps} \end{figure}$ Figure 2: Drift correction for the night of February 27, 2004. Standard stars are shown as open squares and the mean drift as filled circles. The dashed line is the adopted drift as a function of time.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{5756fg3.ps} \end{figure}$ Figure 3: Lithium abundance as a function of $T_{\rm eff}$ . The bold dots denote bona fide members of IC 2391 from Table 8. The circles indicate bona fide members having their Li abundance measured only by Randich et al. (2001). The location of uncertain member 1820 = SHJM 3 (see Sect. 6.2) is marked by the open star. Superimposed dots represent the Pleiades members from Soderblom et al. (1993). It appears that in the range $4600<T_{\rm eff}<4800$ K the cluster stars undergo a rapid phase of Li depletion.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{5756fg4.ps} \end{figure}$ Figure 4: Histogram of mean radial velocities for bona fide cluster members of IC 2391. The dashed line shows a Gaussian fit that peaks at +14.80 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{5756fg5a.eps}\hs... ...e*{3mm} \includegraphics[angle=-90,width=7.2cm,clip]{5756fg5d.eps} \end{figure}$ Figure 5: Examples of cross-correlation function for double-lined spectroscopic binaries found among the FEROS target stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5756fg6.eps} \end{figure}$ Figure 6: Radial-velocity curve for spectroscopic binary star 4413 convolved with the orbital period of P = 90.617 days. The filled squares denote component A; open squares - component B.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg7.ps} \end{figure}$ Figure 7: Color-magnitude diagram for the bona fide members of IC 2391. The bold dots denote single stars or the stars with unknown multiplity status. The open circles indicate spectroscopic binaries. Zero-age main sequence is overplotted using the distance modulus equal to 5.95 mag and zero reddening, E(B-V)=0.0.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg8.ps} \end{figure}$ Figure 8: Color-magnitude diagram for the bona fide members of IC 2391. See Fig. 7 for the meaning of bold dots and open circles. The fit of 30, 40 (dark curve), and 55 Myr isochrones to CMD assuming zero reddening ( E(B-V)=0.0) yields the distance modulus of V₀-M_V=6.01 mag. Our estimate of age is 40 Myr. The location of stars below the 40 Myr isochrone at V>11.5 can be explained by anomalous spectral energy distributions in young K dwarfs.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg9.ps} \end{figure}$ Figure 9: Color-magnitude diagram for bona fide members of IC 2391 using 2MASS $J\!K$ photometry. See Fig. 7 for the meaning of bold dots and open circles. The reddening and distance modulus are the same as in Fig. 7. Two 40 and 100 Myr solar metallicity isochrones from Bonatto et al. (2004) are overplotted.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg10.ps} \end{figure}$ Figure 10: $V\!K$ color-magnitude diagram for bona fide members of IC 2391. See Fig. 7 for the meaning of bold dots and open circles. The reddening and distance modulus are the same as for Fig. 8. The best fit to the lower part of CMD is provided by a 40 Myr isochrone (dark curve). For comparison, 30 and 55 Myr isochrones are also plotted. Similar to $J\!K$ CMD, a fit to the upper part of main sequence is poor most likely for the same reasons as for the CMD from 2MASS photometry (see Fig. 9).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{5756fg11.ps} \end{figure}$ Figure 11: Distribution of $v \sin i$ for bona fide cluster members as a function of B-V, which is roughly inversely proportional to luminosity. The filled circles are new measurements; open circles are those from the literature (fast rotators 1820, 4658, 4757 - likely but not bona fide cluster members - are also included). The distribution is bimodal, peaking at 10 and $\sim$ 80 km s^-1. See Sect. 6.2 about the ultrafast rotator, star 4658.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{5756fg1.eps} \end{figure}$	Figure 1: Proper-motion vector point diagram in the area of IC 2391. A clump of proper motions at $\mu _x=-20.1$ and $\mu _y=+17.6$ mas yr^-1indicates the location of the cluster.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{5756fg2.eps} \end{figure}$	Figure 2: Drift correction for the night of February 27, 2004. Standard stars are shown as open squares and the mean drift as filled circles. The dashed line is the adopted drift as a function of time.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{5756fg4.ps} \end{figure}$	Figure 4: Histogram of mean radial velocities for bona fide cluster members of IC 2391. The dashed line shows a Gaussian fit that peaks at +14.80 km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.2cm,clip]{5756fg5a.eps}\hs... ...e*{3mm} \includegraphics[angle=-90,width=7.2cm,clip]{5756fg5d.eps} \end{figure}$	Figure 5: Examples of cross-correlation function for double-lined spectroscopic binaries found among the FEROS target stars.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5756fg6.eps} \end{figure}$	Figure 6: Radial-velocity curve for spectroscopic binary star 4413 convolved with the orbital period of P = 90.617 days. The filled squares denote component A; open squares - component B.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg7.ps} \end{figure}$	Figure 7: Color-magnitude diagram for the bona fide members of IC 2391. The bold dots denote single stars or the stars with unknown multiplity status. The open circles indicate spectroscopic binaries. Zero-age main sequence is overplotted using the distance modulus equal to 5.95 mag and zero reddening, E(B-V)=0.0.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5756fg9.ps} \end{figure}$	Figure 9: Color-magnitude diagram for bona fide members of IC 2391 using 2MASS $J\!K$ photometry. See Fig. 7 for the meaning of bold dots and open circles. The reddening and distance modulus are the same as in Fig. 7. Two 40 and 100 Myr solar metallicity isochrones from Bonatto et al. (2004) are overplotted.
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