Radial Variation in the Stellar Mass Functions of Star Clusters

A number of recent observational studies of Galactic globular clusters have measured the variation in the slope of a cluster's stellar mass function $α$ with clustercentric distance $r$. In order to gather a deeper understanding of the information contained in such observations, we have explored the evolution of $α(r)$ for star clusters with a variety of initial conditions using a large suite of $N$-body simulations. We have specifically studied how the time evolution of $α(r)$ is affected by initial size, mass, binary fraction, primordial mass segregation, black hole retention, an external tidal field, and the initial mass function itself. Previous studies have shown that the evolution of $α_G$ is closely related to the amount of mass loss suffered by a cluster. Hence for each simulation we have also followed the evolution of the slope of the cluster's global stellar mass function, $α_G$, and have shown that clusters follow a well-defined track in the $α_G$-$dα(r)/d(ln(r/r_m))$ plane. The location of a cluster on the $α_G-dα(r)/d(ln(r/r_m))$ plane can therefore constrain its dynamical history and, in particular, constrain possible variations in the stellar initial mass function. The $α_G$-$dα(r)/d(ln(r/r_m))$ plane thus serves as a key tool for fully exploiting the information contained in wide field studies of cluster stellar mass functions.

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