of NGC 5128 I. Survey and Catalogs'
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Introduction
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Systems of globular clusters are a nearly ubiquitous feature of all nearby galaxies. Globular clusters (GCs), which are typically old with sub-solar metallicities, are the most visible remnants of intense star formation that occurred in a galaxy’s distant past. As single-age, single-metallicity stellar populations, GCs are ideal for studying the fossil remains of a galaxy’s star formation and metal-enrichment history.

The past decade has seen a rapid growth in the study of extragalactic GC systems. The availability of the Hubble Space Telescope (HST) in particular has enabled the study of GC systems in galaxies well beyond the Local Group. One of the more striking results of these studies is the frequency with which the metallicity distributions of these GC systems are bimodal (e.g. Larsen [et al. ]{}2001; Kundu & Whitmore 2001). Different scenarios of galaxy formation (or at least of globular cluster system formation) have been proposed or adapted to explain the observed metallicity distributions and other properties of GC systems: mergers of spiral galaxies (Ashman & Zepf 1992), multiple [*in situ*]{} star formation epochs (Forbes, Brodie, & Grillmair 1997), dissipationless hierarchical merging of protogalactic clumps (Côté, Marzke, & West 