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The autocorrelation function provides an objective test for the existence ofspecial scales in the hierarchical clustering of young stars. We apply thismeasure to single-star photometry for the brightest main sequence stars in theSmall Magellanic Cloud (SMC), the Large Magellanic Cloud (LMC), M33, and M31,using data from the Magellanic Clouds Photometric Survey and the Massey LocalGroup Survey. Our primary result is the identification of a transition to ahigher correlation dimension (weaker clustering) at one kpc in the LMC and M31,and at 300 pc in M33. We suggest that this transition marks the large-scaleregime where disk geometry and dynamics set the scale for structure. On smallerscales, the correlation functions for each galaxy are scale-free over at leasttwo orders of magnitude, with a projected correlation dimension varying from1.0 for M31 to 1.8 for the SMC. This variation is probably caused by acombination of differences in stellar ages and masses, physical environment,and extinction.

Characteristic Scales in Stellar Clustering: A Transition Near the Disk Scale Height