  Correlations between stellar kinematics and chemical abundances are fossil
evidence for evolutionary connections between Galactic structural components.
Extensive stellar surveys show that the only tolerably clear distinction
between galactic components appears in the distributions of specific angular
momentum. Here the stellar metal-poor halo and the metal-rich bulge are
indistinguishable from each other, as are the thick disk and the old disk. Each
pair is very distinct from the other. This leads to an evolutionary model in
which the metal-poor stellar halo evolves into the inner bulge, while the thick
disk is a precursor to the thin disk. These evolutionary sequences are
distinct. The galaxy is made of two discrete `populations', one of low and one
of high angular momentum. Some (minor?) complexity is added to this picture by
the debris of late and continuing mergers, which will be especially important
in the outer stellar halo.
