Fragmentation in Massive Star Formation
Henrik Beuther1* and
Peter Schilke2
Studies of evolved massive stars indicate that they form in
a clustered mode. During the earliest evolutionary stages, these
regions are embedded within their natal cores. Here we present
high-spatial-resolution interferometric dust continuum observations
disentangling the cluster-like structure of a young massive
star–forming region. The derived protocluster mass distribution
is consistent with the stellar initial mass function. Thus,
fragmentation of the initial massive cores may determine the
initial mass function and the masses of the final stars. This
implies that stars of all masses can form via accretion processes,
and coalescence of intermediate-mass protostars appears not
to be necessary.
2 Max-Planck-Institute for Astrophysics, Auf demHuegel 69, 53121 Bonn, Germany.
* To whom correspondence should be addressed. E-mail: hbeuther{at}cfa.harvard.edu
