  Here we present HST WFPC2 imaging of 14 kinematically--distinct core
ellipticals to examine their globular cluster systems. In particular, we probe
the galaxy central regions, for which we might expect to see the strongest
signatures of some formation and destruction processes. These data
substantially increase the number of extragalactic globular cluster systems
studied to date. We find that the globular cluster luminosity, and color, vary
only weakly, if at all, with galactocentric distance. The mean color of
globular clusters are constant with globular cluster magnitude. Several clear
trends are also present. Firstly, globular cluster colors are bluer (more metal
poor by ~ 0.5 dex) than the underlying galaxy starlight at any given
galactocentric distance. Second, we find a correlation over roughly ten
magnitudes between the mean globular cluster metallicity and parent galaxy
luminosity of the form Z goes as L^0.4. This relationship includes dwarf
ellipticals, spiral galaxy bulges and giant ellipticals. Third, we find that
globular cluster surface density distribution can be described by a core model,
for which the core radius correlates with galaxy luminosity. Our results favor
scenarios in which ellipticals form from massive, gas rich progenitors at early
epochs. Detailed simulations of the formation of globular cluster systems would
be valuable to draw firmer conclusions.
