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The observed increase in star formation efficiency with average clouddensity, from several percent in whole giant molecular clouds to ~30 or more incluster-forming cores, can be understood as the result of hierarchical cloudstructure if there is a characteristic density as which individual stars becomewell defined. Also in this case, the efficiency of star formation increaseswith the dispersion of the density probability distribution function (pdf).Models with log-normal pdf's illustrate these effects. The difference betweenstar formation in bound clusters and star formation in loose groupings isattributed to a difference in cloud pressure, with higher pressures formingmore tightly bound clusters. This correlation accounts for the observedincrease in clustering fraction with star formation rate and with theobservation of Scaled OB Associations in low pressure environments. ``Faintfuzzie'' star clusters, which are bound but have low densities, can form inregions with high Mach numbers and low background tidal forces. The proposal byBurkert, Brodie & Larsen (2005) that faint fuzzies form at large radii ingalactic collisional rings, satisfies these constraints.

Variations in Stellar Clustering with Environment: Dispersed Star Formation and the Origin of Faint Fuzzies