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The difference in density profiles of the contributions from differentdensity peaks to dark matter halos results in certain expectations about theMilky Way's stellar halo. We cut our simulated halo stars into two populations:those forming before/during the last major merger, and those accreted after thelast major merger. The former population are more centrally located at z=0,while stars forming in low mass late forming proto-galaxies are spread throughthe halo. A difference in observed binding energy distinguishes these twopopulations. We look at possible chemical abundance signatures of the twopopulations. We also show that galaxies forming in isolated low sigma peakswill form from primordial material. Thus, even though the oldest stars arecentrally concentrated as they originated in the early collapsing, densestregions, primordial stars would be found distributed throughout the halo. Thus,the lack of observed metal free stars can be taken as directly constraining thePopulation III IMF, and the lowest metallicity observed stars can beinterpreted as holding clues to the chemical yields of Pop III stars.

Chemical and Dynamical Properties of the Stellar Halo