HE 0557-4840 - Ultra-Metal-Poor and Carbon-Rich

TL;DR

This paper reports the discovery and detailed spectroscopic analysis of HE 0557-4840, an ultra-metal-poor, carbon-rich star, providing insights into early Galactic chemical enrichment and the distribution of extremely metal-poor stars.

Contribution

It presents the discovery of HE 0557-4840 as the third most metal-poor star, expanding understanding of the metallicity distribution and chemical properties of the earliest stars.

Findings

HE 0557-4840 has [Fe/H] = -4.75, making it one of the most metal-poor stars known.

The star is carbon-rich with [C/Fe] = +1.6, consistent with trends at low metallicity.

HE 0557-4840's abundance pattern suggests early chemical enrichment involved mixing and fallback processes.

Abstract

We report the discovery and high-resolution, high S/N, spectroscopic analysis of the ultra-metal-poor red giant HE 0557-4840, which is the third most heavy-element deficient star currently known. Its atmospheric parameters are T_eff = 4900 K, log g = 2.2, and [Fe/H]= -4.75. This brings the number of stars with [Fe/H] < -4.0 to three, and the discovery of HE 0557-4840 suggests that the metallicity distribution function of the Galactic halo does not have a "gap" between [Fe/H] = -4.0, where several stars are known, and the two most metal-poor stars, at [Fe/H] ~ -5.3. HE 0557-4840 is carbon rich - [C/Fe] = +1.6 - a property shared by all three objects with [Fe/H] < -4.0, suggesting that the well-known increase of carbon relative to iron with decreasing [Fe/H] reaches its logical conclusion - ubiquitous carbon richness - at lowest abundance. We also present abundances (nine) and limits (nine) for a further 18 elements. For species having well-measured abundances or strong upper limits, HE 0557-4840 is "normal" in comparison with the bulk of the stellar population at [Fe/H] ~ -4.0 - with the possible exception of Co. We discuss the implications of these results for chemical enrichment at the earliest times, in the context of single ("mixing and fallback") and two-component enrichment models. While neither offers a clear solution, the latter appears closer to the mark. Further data are required to determine the oxygen abundance and improve that of Co, and hence more strongly constrain the origin of this object.