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We perform a series of three-dimensional, magnetohydrodynamical (MHD)simulations of star cluster formation including gravity, turbulence, magneticfields, stellar radiative heating and outflow feedback. We observe that theinclusion of protostellar outflows (1) reduces the star formation rate by afactor of $\sim2$, (2) increases fragmentation, and (3) shifts the initial massfunction (IMF) to lower masses by a factor of $2.0\pm0.2$, withoutsignificantly affecting the overall shape of the IMF. The form of the sinkparticle (protostellar objects) mass distribution obtained from our simulationsmatches the observational IMFs reasonably well. We also show thatturbulence-based theoretical models of the IMF agree well with our simulationIMF in the high-mass and low-mass regime, but do not predict any brown dwarfs,whereas our simulations produce a considerable number of sub-stellar objects,which are produced by dynamical interactions (ejections). We find that thesedynamical interactions also play a key role for the binary separationdistribution and stellar kinematics in general. Our numerical model of starcluster formation also reproduces the observed mass dependence of multiplicity.Our multiplicity fraction estimates generally concur with the observationalestimates for different spectral types. We further calculate the specificangular momentum of all the sink particles and find that the average value of$1.5 \times 10^{19}\, \mathrm{cm^2\, s^{-1}}$ is consistent with observationaldata. The specific angular momentum of our sink particles lies in the rangetypical of protostellar envelopes and binaries. We conclude that the IMF iscontrolled by a combination of gravity, turbulence, magnetic fields, radiationand outflow feedback.

The IMF and multiplicity of stars from gravity, turbulence, magnetic fields, radiation and outflow feedback