|Authors||Richard de Grijs1, Mark I. Wilkinson2, Clive N. Tadhunter1|
|Affiliation||1 Department of Physics & Astronomy, The University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK; 2 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK|
|Accepted by||Monthly Notices of the Royal Astronomical Society|
We evolve the luminosities of those young massive star clusters (YMCs) in the local Universe which have velocity dispersion measurements to an age of 12 Gyr, adopting a variety of IMF descriptions, and find that most YMCs will evolve to loci close to, or to slightly fainter luminosities than the improved GC relationship. In the absence of significant external disturbances, this implies that these objects may potentially survive to become old GC-type objects over a Hubble time. The main advantage of our new method is its simplicity. Where alternative methods, based on dynamical mass estimates, require one to obtain accurate size estimates and to make further assumptions, the only observables required here are the system's velocity dispersion and luminosity. The most important factor affecting the robustness of our conclusions is the adopted form of the initial mass function. We use the results of N-body simulations to confirm that dynamical evolution of the clusters does not significantly alter our conclusions about the likelihood of individual clusters surviving to late times. Finally, we find that our youngest observed clusters are consistent with having evolved from a relation of the form LV/Lo ~ sigma02.1 (km/s). This relation may actually correspond to the origin of the GC fundamental plane.