Implications and Applications of Kinematic Galaxy Scaling Relations
Figure 8
The evolution of as inferred from early-type galaxies and comparison between models and our cluster data. The stellar cluster data are plotted in solid circles (black), the results obtained using the results from van Dokkum and Conroy [72] are plotted with open circles (red) when normalized to match the results from the sample of Graves et al. [73], which are plotted with squares (pink). Also shown are the van Dokkum and Conroy [72] data assuming a dark matter fraction of 80%, so as to qualitatively match to the stellar cluster data, in open circles (blue). The dark matter fraction is likely to be somewhere between 0 and 80%. The upper solid line represents the values of from a PEGASE model of a population with an instantaneous burst at and a Salpeter IMF, while the lower represents a model with a light-weighted Kroupa IMF.
