Variation in the stellar mass function along stellar streams

Stellar streams are the inevitable end product of star cluster evolution, with properties a given stream being related to its progenitor. We consider how dynamical history progenitor cluster, as traced by evolution stellar mass function, is reflected in resultant stream. generate model evolving clusters range initial half-mass relaxation times and dissolution via direct N-body simulations. that dissolve quickly show no variation function along Variation is, however, observed after several times. The at edges approximately primordial it populated first stars escape before segregation occurs. Moving inwards steepens intermediate parts consist mostly low-mass escaped some has occurred. centre then marked flatter region dominated high-mass segregated cluster's were last become unbound. further find maximum slope rate which decreases distance from dissolved serve proxies for state reached dissolution; this may be able applied near-future observations.