All Figures

	Figure 1: The globular clusters analyzed in this data set. Small dots represent optically detected globular clusters, while the larger open circles surround the clusters with X-ray sources.
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In the text

	Figure 2: Metallicity corrected LMXB probability as a function of mass, fit using binning, with 7 bins. Fits with different numbers of bins produce results which are the same within statistical errors. Changing the metallicity correction between 0.20 and 0.30 has no effect on the mass exponent, as expected given the absence of correlations between cluster mass and metallicity.
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In the text

	Figure 3: Binned collision rate versus mass for the Milky Way's globular clusters, using data from the Harris catalog with 8 bins.
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In the text

	Figure 4: Binned values of versus mass for the Milky Way's globular clusters, using data from the Harris catalog with 6 bins.
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In the text

	Figure 5: The retention fraction as a function of mass, fitted to the King-model data with a constant kick velocity distribution between 0 and 1000 km s-1. Chi-square was minimized to obtain the fit.
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In the text