Derived parameters & abundances of metal-poor stars

All of these stars had their parameters previously published by Roederer et al. We use color-Teff relationships calibrated for Gaia and 2MASS photometry to calculate improved effective temperatures (Teff). We calculate log of surface gravity (log g) values using measurements derived from Gaia parallaxes and other fundamental stellar properties.

We perform a standard LTE abundance analysis using MARCS model atmospheres and the MOOG line analysis software to rederive microturbulence velocity parameters, metallicities, and abundances based on O i, Na i, Mg i, Si i, K i, Ca i, Ti i, Ti ii, Cr i, Cr ii, Fe i, Fe ii, Ni i, and Zn i lines using previously measured equivalent widths. On average, the new Teff values are 310K warmer, the new log g values are higher by 0.64dex, and the new [Fe/H] values are higher by 0.26dex.