  The goal of this investigation is to reconstruct the cosmic star formation
rate density history from local observations and in doing so to gain insight
into how galaxies might have formed and evolved. A new chemical evolution model
is described which accounts for the formation of globular clusters as well as
the accompanying field stars. When this model is used in conjunction with the
observed age metallicity relations for the clusters and with input which allows
for the formation of the nearly universally observed bimodal distribution of
globular clusters, star formation rates are obtained. By confining attention to
a representative volume of the local universe, these rates allow a successful
reconstruction of the Madau plot while complementary results similtaneously
satisfy many local cosmological constraints. A physical framework for galaxy
formation is presented which incorporates the results from this chemical
evolution model and assumes an anisotropic collapse. In addition to providing
the `classical' halo, bulge and disk components, the model also predicts a new
stellar halo component with peak [Fe/H] ~ -0.8 and disk-like angular momentum
and allows for the formation of a thick disk as outlined by the group of metal
rich globular clusters. Milky Way counterparts of the latter two components are
identified.
