Fragmentation of a high-mass star-forming core

Abstract

At the earliest evolutionary stages, massive star-forming regions are deeply embedded within their natal cores and not observable at optical and near-infrared wavelengths. Interferometric high-spatial resolution mm dust continuum observations of one very young high-mass star-forming region disentangle its cluster-like nature already at the very beginning of the star formation process. The derived protocluster mass function is consistent with the stellar IMF. Hence, fragmentation of the initial massive cores may determine the IMF and the masses of the final stars. This implies that stars of all masses can form via accretion, and coalescence of protostars appears not to be necessary.