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This paper investigates the discrepancy between recent measurements of thedensity profile of the globular cluster 47 Tuc that have used HST data sets.Guhathakurta et al. (1992) used pre-refurbishment WFPC1 V-band images to deriver_c = 23" +/- 2". Calzetti et al. (1993) suggested that the density profile isa superposition of two King profiles (r_c = 8" and r_c = 25") based on U-bandFOC images. De Marchi et al. (1996) used deep WFPC1 U-band images to derive r_c= 12" +/- 2". Differences in the adopted cluster centers are not the cause ofthe discrepancy. Our independent analysis of the data used by De Marchi et al.reaches the following conclusions: (1) De Marchi et al.'s r_c ~ 12" value isspuriously low, a result of radially-varying bias in the star counts in amagnitude limited sample -- photometric errors and a steeply rising stellarluminosity function cause more stars to scatter across the limiting magnitudeinto the sample than out of it, especially near the cluster center wherecrowding effects are most severe. (2) Changing the limiting magnitude to themain sequence turnoff, away from the steep part of the luminosity function,partially alleviates the problem and results in r_c = 18". (3) Combining such alimiting magnitude with accurate photometry derived from PSF fitting, insteadof the less accurate aperture photometry employed by De Marchi et al., resultsin a reliable measurement of the density profile which is well fit by r_c = 22"+/- 2". Archival WFPC2 data are used to derive a star list with a higher degreeof completeness, greater photometric accuracy, and wider areal coverage thanthe WFPC1 and FOC data sets; the WFPC2-based density profile supports the aboveconclusions, yielding r_c = 24" +/- 1.9".

Resolving the Controversy over the Core Radius of 47 Tucanae (NGC 104)1,2