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Intracluster stellar populations are a natural result of tidal interactionsin galaxy clusters. Measuring these populations is difficult, but important forunderstanding the assembly of the most massive galaxies. The Coma cluster isone of the nearest truly massive galaxy clusters, and is host to acorrespondingly large system of globular clusters (GCs). We use imaging fromthe HST/ACS Coma Cluster Survey to present the first definitive detection of alarge population of intracluster GCs (IGCs) that fills the Coma cluster coreand is not associated with individual galaxies. The GC surface density profilearound the central massive elliptical galaxy, NGC 4874, is dominated at largeradii by a population of IGCs that extend to the limit of our data (R<520 kpc).We estimate that there are 47000+/-1600 (random) +4000/-5000 (systematic) IGCsout to this radius, and that they make up ~70% of the central GC system, makingthis the largest GC system in the nearby Universe. Even including the GCsystems of other cluster galaxies, IGCs still make up ~30-45% of the GCs in thecluster core. Observational limits from previous studies of the intraclusterlight (ICL) suggest that the IGC population has a high specific frequency. Ifthe IGC population has a specific frequency similar to high-S_N dwarf galaxies,then the ICL has a total stellar mass of ~10^12 M_sun within the cluster core.The ICL makes up approximately half of the stellar luminosity and one-third ofthe stellar mass of the central (NGC4874+ICL) system. The color distribution ofthe IGC population is bimodal, with blue, metal-poor GCs outnumbering red,metal-rich GCs by a ratio of 4:1. The fraction of red IGCs (20%), and the redcolor of those GCs, implies that IGCs can originate from the halos ofrelatively massive, L* galaxies, and not solely from the disruption of dwarfgalaxies. (Abridged)

The HST/ACS Coma Cluster Survey IV. Intergalactic Globular Clusters and the Massive Globular Cluster System at the Core of the Coma Galaxy Cluster