HE 1327−2326, an Unevolved Star with [Fe/H]<−5.0. II. New 3D−1D Corrected Abundances from a Very Large Telescope UVES Spectrum

We present a new abundance analysis of HE 1327–2326, which is currently the most iron-poor star, based on observational data obtained with the VLT Ultraviolet and Visual Echelle Spectrograph (UVES). We correct the one-dimensional (1D) LTE abundances for three-dimensional (3D) effects to provide an abundance pattern that supersedes previous works and should be used to observationally test current models of the chemical yields of the first-generation supernovae (SNe). Apart from confirming the 1D LTE abundances found in previous studies before accounting for 3D effects, we make use of a novel technique to apply the 3D–1D corrections for CNO which are a function of excitation potential and line strength for the molecular lines that comprise the observable CH, NH, and OH features. We find that the fit to the NH band at 3360 Å is greatly improved due to the application of the 3D–1D corrections. This may indicate that 3D effects are actually observable in this star. We also report the first detection of several weak Ni lines. The cosmologically important element Li is still not detected; the new Li upper limit is extremely low, A (Li) < 0.62, and in stark contrast with results not only from the Wilkinson Microwave Anisotropy Probe ( WMAP ) but also from other metal-poor stars. We also discuss how the new corrected abundance pattern of HE 1327–2326 is being reproduced by individual and integrated yields of SNe.