Radial distribution of the population ratio N_BSS/N_HB for M5, M3, 47 Tuc, and NGC 6752, plotted as a function of the radial distance from the cluster center, normalized to the core radius r_c (from Mapelli et al. 2006, ﹩r_{c}\simeq 30^{\prime \prime }﹩, 21^{﹩\arcsec﹩}, 28^{﹩\arcsec﹩} for M3, 47 Tuc, and NGC 6752, respectively). The arrows indicate the position of the minimum of the distribution in each case. The outermost point shown for M5 (open circle) corresponds to BSS 58, lying at ﹩r\simeq 995^{\prime \prime }﹩. This star has not been considered in the quantitative study of the BSS radial distribution since only a negligible fraction of the annuls between 800^{﹩\arcsec﹩} and r_t is sampled by our observations.