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Most of the more massive galaxies in the Local Group contain one or several globular clusters,resulting in a variety of different specific frequencies.These globular clusters span a wide range of metallicities.While they are all “old”,age differences of several Gyr are found.Some galaxies,such as the Magellanic Clouds,also host intermediate-age globular cluster candidates.The structural properties of globular clusters differ widely and appear to be strongly influenced by their environment,ranging from primarily compact,massive clusters in the central regions of massive galaxies to more extended clusters in their outskirts or in dwarf galaxies.A few globular clusters are observed in early or advanced stages of tidal disruption.A considerable fraction of the outer halo globular cluster population of galaxies like the Milky Way may have been accreted from since disrupted satellites.However,the second-parameter dichotomy is also prevalent in dwarf galaxies,and thus far no extremely metal-deficient globular cluster has been found,suggesting that they are somewhat younger than the oldest field populations.The internal dynamics of distant globular clusters analyzed thus far are consistent with stellar Newtonian dynamics,suggesting neither the presence of dark matter nor a need for modified gravitational theories.In dwarf galaxies,the overall globular cluster dynamics support cored dark matter halo profiles for the host galaxies.