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The fraction of binary stars is an important ingredient to interpret globularcluster dynamical evolution and their stellar population. We investigate theproperties of main-sequence binaries measured in a uniform photometric sampleof 59 Galactic globular clusters that were observed by HST WFC/ACS as a part ofthe Globular Cluster Treasury project. We measured the fraction of binaries andthe distribution of mass-ratio as a function of radial location within thecluster, from the central core to beyond the half-mass radius. We studied theradial distribution of binary stars, and the distribution of stellar massratios. We investigated monovariate relations between the fraction of binariesand the main parameters of their host clusters. We found that in nearly all theclusters, the total fraction of binaries is significantly smaller than thefraction of binaries in the field, with a few exceptions only. Binary stars aresignificantly more centrally concentrated than single MS stars in most of theclusters studied in this paper. The distribution of the mass ratio is generallyflat (for mass-ratio parameter q>0.5). We found a significant anti-correlationbetween the binary fraction in a cluster and its absolute luminosity (mass).Some, less significant correlation with the collisional parameter, the centralstellar density, and the central velocity dispersion are present. There is nostatistically significant relation between the binary fraction and othercluster parameters. We confirm the correlation between the binary fraction andthe fraction of blue stragglers in the cluster.

The ACS Survey of Galactic Globular Clusters. XII. Photometric Binaries along the Main-Sequence