The devil is in the tails: the role of globular cluster mass evolution on stream properties

We present a study of the effects of collisional dynamics on the formation and detectability cold tidal streams. A semi-analytical model for the evolution of the stellar mass function implemented and coupled to a fast stellar stream simulation code, as well as the synthetic evolution code EMACSS for the mass evolution as a function of a globular cluster . We find that the increase in the average mass of the escaping stars for clusters close dissolution has a major effect on the observable stream surface density. As an example, show that Palomar 5 would have undetectable streams (in an SDSS-like survey) if it was three times more massive, despite the fact that a more massive cluster loses stars a higher rate. This bias due to the preferential escape of low-mass stars is an alternative for the absence of tails near massive clusters, than a dark matter halo associated the cluster. We explore the orbits of a large sample of Milky Way globular clusters and their initial masses and remaining mass fraction. Using properties of known tidal tails explore regions of parameter space that favour the detectability of a stream. A list of high candidates is discussed.