  We investigate the relation of the stellar initial mass function (IMF) and
the dense core mass function (CMF), using stellar masses and positions in 14
well-studied young groups. Initial column density maps are computed by
replacing each star with a model initial core having the same star formation
efficiency (SFE). For each group the SFE, core model, and observational
resolution are varied to produce a realistic range of initial maps. A
clumpfinding algorithm parses each initial map into derived cores, derived core
masses, and a derived CMF. The main result is that projected blending of
initial cores causes derived cores to be too few and too massive. The number of
derived cores is fewer than the number of initial cores by a mean factor 1.4 in
sparse groups and 5 in crowded groups. The mass at the peak of the derived CMF
exceeds the mass at the peak of the initial CMF by a mean factor 1.0 in sparse
groups and 12.1 in crowded groups. These results imply that in crowded young
groups and clusters, the mass distribution of observed cores may not reliably
predict the mass distribution of protostars which will form in those cores.
