  Globular clusters rotate significantly, and with the increasing amount of
detailed morphologicaland kinematical data obtained in recent years on galactic
globular clusters many interesting features show up. We show how our
theoretical evolutionary models of rotating clusters can be used to obtain
fits, which at least properly model the overall rotation and its implied
kinematics in full 2D detail (dispersions, rotation velocities). Our simplified
equal mass axisymmetric rotatingmodel provides detailed two-dimensional
kinematical and morphological data for star clusters. The degree of rotation is
not dominant in energy, but also non-negligible for the phase space
distribution function, shape and kinematics of clusters. Therefore the models
are well applicable for galactic globular clusters. Since previously published
papers on that matter by us made it difficult to do detailed comparisons with
observations we provide a much more comprehensive and easy-to-use set of data
here, which uses as entries dynamical age and flattening of observed cluster
andthen offers a limited range of applicable models in full detail. The method,
data structure and some exemplary comparison with observations are presented.
Future work will improve modelling anddata base to take a central black hole, a
mass spectrum and stellar evolution into account.
