SIMBAD references

We show that the globular cluster mass function (GCMF) in the Milky Way depends on cluster half-mass density, ρ_h, in the sense that the turnover mass M_TO increases with ρ_hwhile the width of the GCMF decreases. We argue that this is the expected signature of the slow erosion of a mass function that initially rose toward low masses, predominantly through cluster evaporation driven by internal two-body relaxation. We find excellent agreement between the observed GCMF–including its dependence on internal density ρ_h, central concentration c, and Galactocentric distance r_gc–and a simple model in which the relaxation-driven mass-loss rates of clusters are approximated by -dM/dt=µ_ev∝ρ^1/2_h. In particular, we recover the well-known insensitivity of M_TO to r_gc. This feature does not derive from a literal ``universality'' of the GCMF turnover mass, but rather from a significant variation of M_TO with ρ_h–the expected outcome of relaxation-driven cluster disruption–plus significant scatter in ρ_h as a function of r_gc. Our conclusions are the same if the evaporation rates are assumed to depend instead on the mean volume or surface densities of clusters inside their tidal radii, as µ_ev∝ρ^1/2_t or µ_ev∝Σ^3/4_t–alternative prescriptions that are physically motivated but involve cluster properties (ρ_t and Σ_t) that are not as well defined or as readily observable as ρ_h. In all cases the normalization of µ_ev required to fit the GCMF implies cluster lifetimes that are within the range of standard values (although falling toward the low end of this range). Our analysis does not depend on any assumptions or information about velocity anisotropy in the globular cluster system.