SIMBAD references

We present an elemental-abundance analysis of an extremely metal-poor (EMP; [Fe/H] V=12.14, is the lowest metallicity star found in the pre-survey, and is one of only ∼20 known EMP stars that are this bright or brighter. Our high-resolution spectroscopic analysis shows that this star is a subgiant with [Fe/H]=-3.42, having 'normal' carbon and no enhancement of neutron-capture abundances. Strontium is underabundant, [Sr/Fe]=-0.47, but the derived lower limit on [Sr/Ba] indicates that Sr is likely enhanced relative to Ba. This star belongs to the sparsely populated class of α-poor EMP stars that exhibit low ratios of [Mg/Fe], [Si/Fe], and [Ca/Fe] compared to typical halo stars at similar metallicity. The observed variations in radial velocity from several epochs of (low- and high-resolution) spectroscopic follow-up indicate that SDSS J134338.67+484426.6 is a possible long-period binary. We also discuss the abundance trends in EMP stars for r-process elements, and compare with other magnesium-poor stars.