Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig1.ps}\end{figure}$ Figure 1: The filled circles give estimated values of $\alpha _{\rm turb}$ (the ratio of turbulent to gravitational energy, see Eq. (1)) and $M_{\rm core}$ (core mass) for the starless cores in the Jijina et al. (1999) catalogue. The hatched region gives the range of $(\alpha _{\rm turb},M_{\rm core})$ values used in this paper (i.e. $0 \leq \alpha _{\rm turb} \leq 0.25$ and $M_{\rm core} = 5.4 ~M_\odot$ ). The cross (+) and the star (*) give - respectively - the $(\alpha _{\rm turb},M_{\rm core})$ values used by Bate et al. (2002a,b, 2003) and Delgado Donate et al. (2003a,b).
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig2.ps}\end{figure}$ Figure 2: The average number of objects formed in a core, $\left <{\cal N}_{\rm obj}\right >$ , as a function of the ratio of turbulent to gravitational energy $\alpha _{\rm turb}$ . The error bars give the standard deviation (see Eq. (5)).
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{02... ...ludegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig3c.ps}\end{figure}$ Figure 3: The normalized mass functions for $\alpha _{\rm turb} = 0.05$ (top), 0.10 (middle) and 0.25 (bottom). The shaded regions show stars in stable multiple systems, the hashed regions show stars in unstable multiple systems, and the open regions show single stars.
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig4.ps}\end{figure}$ Figure 4: The combined (and un-normalized) mass function for all the simulations having $\alpha _{\rm turb} \geq 0.05$ , (i.e. $\alpha_{\rm turb} = 0.05~(\times 20)$ , $0.10~(\times 20)\;{\rm and}\;0.25~(\times 10)$ ), this being an approximation to the distribution of $\alpha _{\rm turb}$ values in the Taurus star formation region. The error bars give ${\pm}\!\sqrt{N}$ uncertainties. The dotted lines show separate fits to the unbound objects (the flat distribution at low mass) and the bound objects (the log-normal distribution at high mass); parameter fits are given in the main text). The dashed line shows the combination of these two separate fits.
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{02... ...ludegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig5c.ps}\end{figure}$ Figure 5: The histograms show the cumulative distribution functions of semi-major axes for the ensembles with $\alpha _{\rm turb} = 0.05$ (top), 0.10 (middle) and 0.25 (bottom). The dashed line shows the Gaussian fit to the DM91 period distribution.
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.45cm,angle=270,clip]{0285fig6.ps}\end{figure}$ Figure 6: For each binary system, the semi-major axis, a is plotted against the number of objects formed in that simulation, $N_{\rm obj}$ , with open circles for for $\alpha _{\rm turb} = 0.05$ , filled circles for $\alpha _{\rm turb}=0.10$ , and stars for $\alpha _{\rm turb}=0.25$ . The average semi-major axis, $\bar{a}$ , decreases with increasing $N_{\rm obj}$ , due to dynamical hardening. To the left of the dashed line at $a = 5~{\rm au}$ the a-values are upper limits, due to gravity softening.
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig7.ps}\end{figure}$ Figure 7: The distribution of mass ratios for simulations with $\alpha _{\rm turb} = 0.05$ (filled), $\alpha _{\rm turb}=0.10$ (hashed) and $\alpha _{\rm turb}=0.25$ (open). (Note that the number of simulations in the $\alpha _{\rm turb}=0.25$ ensemble is only half of the number in the other ensembles.)
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig8.ps}\end{figure}$ Figure 8: The cumulative distribution function of eccentricities for all simulations with $\alpha _{\rm turb} \geq 0.05$ . The dashed line shows the DM91 fit of a linearly increasing eccentricity distribution.
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In the text

$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig2.ps}\end{figure}$	Figure 2: The average number of objects formed in a core, $\left <{\cal N}_{\rm obj}\right >$ , as a function of the ratio of turbulent to gravitational energy $\alpha _{\rm turb}$ . The error bars give the standard deviation (see Eq. (5)).
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$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{02... ...ludegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig3c.ps}\end{figure}$	Figure 3: The normalized mass functions for $\alpha _{\rm turb} = 0.05$ (top), 0.10 (middle) and 0.25 (bottom). The shaded regions show stars in stable multiple systems, the hashed regions show stars in unstable multiple systems, and the open regions show single stars.
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$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{02... ...ludegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig5c.ps}\end{figure}$	Figure 5: The histograms show the cumulative distribution functions of semi-major axes for the ensembles with $\alpha _{\rm turb} = 0.05$ (top), 0.10 (middle) and 0.25 (bottom). The dashed line shows the Gaussian fit to the DM91 period distribution.
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$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig7.ps}\end{figure}$	Figure 7: The distribution of mass ratios for simulations with $\alpha _{\rm turb} = 0.05$ (filled), $\alpha _{\rm turb}=0.10$ (hashed) and $\alpha _{\rm turb}=0.25$ (open). (Note that the number of simulations in the $\alpha _{\rm turb}=0.25$ ensemble is only half of the number in the other ensembles.)
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$\begin{figure} \par\includegraphics[height=12.1cm,width=7.4cm,angle=270,clip]{0285fig8.ps}\end{figure}$	Figure 8: The cumulative distribution function of eccentricities for all simulations with $\alpha _{\rm turb} \geq 0.05$ . The dashed line shows the DM91 fit of a linearly increasing eccentricity distribution.
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