All Figures

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1898fig1.eps} \end{figure}$ Figure 1: The temporal evolution of the fractions of YSO classes for three models: M2k4 ( left), M6k2a ( middle), and M10k2 (right), upper panel: absolute numbers, lower panel: relative numbers. Solid line: Class 0, dashed line: Class 1, long dashed line: Class 2+3, dotted line: prestellar cores (only shown in the upper panel). The abscissa gives the time in units of the global free-fall time. The zero point of the timescale corresponds to the time when gravity is "switched on''. Note the different intervals covered in the models. The vertical lines in the lower panel indicate the time $\tau$ , when the model shows the best agreement with the observations of Serpens (dotted), NGC 7129 (dashed), Taurus and IC 1396A (dash-dotted), $\rho$ Ophiuchi (long dashes), Cha I (dash dot dot dot), and IC 348 (second dotted line). Because of similar relative YSO numbers, the best-fit evolutionary times for Taurus and IC 1396A are essentially indistinguishable.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1898fig2.eps} \end{figure}$ Figure 2: The time $\tau$ of the best correspondence between models and observations (in units of the global free-fall time $\tau _{\rm ff}$ ) for the seven investigated clusters. The symbols denote the parameters of the models: $\mathcal{M} = 0.5$ (triangles), $\mathcal{M} = 2$ (triangles down), $\mathcal{M} = 3.2$ (squares), $\mathcal{M} = 6$ (diamonds), $\mathcal{M} = 10$ (stars); $1 \le k \le 2$ (open symbols), $3 \le k \le 4$ (grey symbols), $7 \le k \le 8$ (filled symbols). The Gaussian collapse models are displayed as asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1898fig3.eps} \end{figure}$ Figure 3: The star formation efficiency at time $\tau$ plotted versus the Mach number of the models. The symbols are the same as in Fig. 2, circles denote models with $\mathcal{M} = 0.1$ . The dotted lines show a linear fit to the data.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1898fig3.eps} \end{figure}$	Figure 3: The star formation efficiency at time $\tau$ plotted versus the Mach number of the models. The symbols are the same as in Fig. 2, circles denote models with $\mathcal{M} = 0.1$ . The dotted lines show a linear fit to the data.
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