All Figures

	Figure 1: A plot of number of stars, N, versus logarithmic stellar mass, , comparing the IMF in Taurus (solid-line histogram, adapted from Luhman et al. 2003a) with that in Orion (shaded histogram, adapted from Muench et al. 2002). The Orion IMF is normalised to have the same number of stars as the Taurus IMF. The two IMFs are clearly different.
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In the text

Figure 2: The stellar IMF produced from an ensemble of fifty core collapse simulations is shown as a solid-line histogram. This histogram is well-fitted by the sum (dashed line) of two distributions (dotted lines): a log-normal distribution with mean and standard deviation plus a flat distribution below The stars making up the log-normal distribution generally tend to remain in multiple systems, whilst those making up the flat distribution are generally objects that have been ejected from multiple systems.

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In the text

Figure 3: The solid-line histogram shows the observed IMF of Taurus due to Luhman et al. (2003a) (as in Fig. 1). The shaded histogram shows the model IMF from Fig. 2, normalised and rebinned to match the binning of Luhman et al. (2003a). The model IMF was produced from an ensemble of simulations which starts with the observed core mass distribution in Taurus and initial conditions for individual cores (density profile, level of turbulence, etc.) based on the physical conditions observed in pre-stellar cores in Taurus. The two histograms have been normalised by minimising . Agreement between the model and the observations is good (see text for discussion).

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In the text