A New Population of Old Stars

We report the results of a coherent study of three chemically anomalous metal-poor ([Fe/H] ∼ –2) stars. These objects exhibit unusually low abundances of Mg, Si, Ca (α-elements) and Sr, Y, and Ba (neutron-capture elements). Our analyses confirm and expand upon earlier reports of atypical abundances in BD+80 245, G4-36, and CS22966-043. We also find that the latter two stars exhibit enhanced abundances of Cr, Mn, Ni, and Zn (iron-peak elements), along with what appears to be large abundances of Ga, with respect to the abundance of iron. Comparing the chemical abundances of these stars to supernova model yields, we derive supernovae ratios of Type Ia versus Type II events in the range of 0.6 ≤ (NIa/NII)NewPop ≤ 1.3. Whereas, for the Sun, we derive supernovae ratios in good agreement with those found in the literature: 0.18 ± 0.01 < (NIa/NII)⊙ < 0.25 ± 0.06. Given the relatively low metallicity and high (NIa/NII) ratios of the low-α stars studied here, these objects may have witnessed, or been born from material produced in the yields of the earliest supernova Type Ia events. 1.