  The relations between the luminosities $M_{V}$, the metallicities $[Fe/H]$,
the Galactocentric radii $R$, and the central concentration indices $c$ of
Galactic globular clusters are discussed. It is found that the most luminous
clusters rarely have collapsed cores. The reason for this might be that the
core collapse time scales for such populous clusters are greater than the age
of the Galaxy. Among those clusters, for which the structure has not been
modified by core collapse, there is a correlation between central concentration
and integrated luminosity, in the sense that the most luminous clusters have
the strongest central concentration. The outermost region of the Galaxy with
$R>10$ kpc was apparently not able to form metal-rich $([Fe/H]>-1.0)$ globular
clusters, whereas such clusters (of which Ter 7 is the prototype) were able to
form in some nearby dwarf spheroidal galaxies. It is not yet clear how the
popular hypothesis that globular clusters were initially formed with a single
power law mass spectrum can be reconciled with the observation that both (1)
Galactic globular clusters with $R>80$ kpc, and (2) the globulars associated
with the Sagittarius dwarf, appear to have bi-modal luminosity functions.
