2004ApJ...603..108H

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 that 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 that 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 simultaneously satisfy many local cosmological constraints. A physical framework for galaxy formation is presented that 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 disklike 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.