The Most Metal-Poor Stars. IV. The Two Populations With [Fe/H] < -3.0

TL;DR

This study analyzes the chemical compositions of extremely metal-poor Galactic halo stars, identifying two populations distinguished by carbon content and proposing different early Universe cooling mechanisms as their origin.

Contribution

It provides a detailed chemical abundance analysis of stars with [Fe/H] < -3.0, revealing two distinct populations and suggesting different formation pathways in the early Universe.

Findings

C-rich stars constitute ~28% of stars below [Fe/H] = -3.1.

C-rich stars are O-rich and show enhanced Na, Mg, Al.

Limited radial velocity data do not strongly support binarity as a key factor.

Abstract

We discuss the carbon-normal and carbon-rich populations of Galactic halo stars having [Fe/H] < -3.0, utilizing chemical abundances from high-resolution, high-S/N model-atmosphere analyses. The C-rich population represents ~28% of stars below [Fe/H] = -3.1, with the present C-rich sample comprising 16 CEMP-no stars, and two others with [Fe/H] ~ -5.5 and uncertain classification. The population is O-rich ([O/Fe] > +1.5); the light elements Na, Mg, and Al are enhanced relative to Fe in half the sample; and for Z > 20 (Ca) there is little evidence for enhancements relative to solar values. These results are best explained in terms of the admixing and processing of material from H-burning and He-burning regions as achieved by nucleosynthesis in zero-heavy-element models in the literature of "mixing and fallback" supernovae (SNe); of rotating, massive and intermediate mass stars; and of Type II SNe with relativistic jets. The available (limited) radial velocities offer little support for the C-rich stars with [Fe/H] < -3.1 being binary. More data are required before one could conclude that binarity is key to an understanding of this population. We suggest that the C-rich and C-normal populations result from two different gas cooling channels in the very early Universe, of material that formed the progenitors of the two populations. The first was cooling by fine-structure line transitions of CII and OI (to form the C-rich population); the second, while not well-defined (perhaps dust-induced cooling?), led to the C-normal group. In this scenario, the C-rich population contains the oldest stars currently observed.