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We present evidence for mass segregation in the outer-halo globular clusterPalomar 14, which is intuitively unexpected since its present-day two-bodyrelaxation time significantly exceeds the Hubble time. Based on archival HubbleSpace Telescope imaging, we analyze the radial dependence of the stellar massfunction in the cluster's inner 39.2 pc in the mass range of 0.53-0.80 M_sun,ranging from the main-sequence turn-off down to a V-band magnitude of 27.1 mag.The mass function at different radii is well approximated by a power law andrises from a shallow slope of 0.6+/-0.2 in the cluster's core to a slope of1.6+/-0.3 beyond 18.6 pc. This is seemingly in conflict with the finding byBeccari et al. (2011), who interpret the cluster's non-segregated population of(more massive) blue straggler stars, compared to (less massive) red giants andhorizontal branch stars, as evidence that the cluster has not experienceddynamical segregation yet. We discuss how both results can be reconciled. Ourfindings indicate that the cluster was either primordially mass-segregatedand/or used to be significantly more compact in the past. For the latter case,we propose tidal shocks as the mechanism driving the cluster's expansion, whichwould imply that Palomar 14 is on a highly eccentric orbit. Conversely, if thecluster formed already extended and with primordial mass segregation, thiscould support an accretion origin of the cluster.

Mass segregation in the outer halo globular cluster Palomar 14