Open Access
Table C.1
Summary of the timeline, the chemical features, and the origin of the different populations in ωCen.
| Timeline | Chemical features | Origin |
|---|---|---|
| 1P | Similar to Galactic halo stars, with a small iron spread. | Formed from a primordial cloud. |
| AI | Enriched in C+N+O (primarily due to C and O), α-elements, iron, and s-process elements, relative to 1P stars. | Medium polluted by ejecta from CCSNe (and possibly other massive stars). |
| 2P (upper stream) | Depleted in Li, C, O, and Mg; enriched in N, Na, Al, and Si relative to 1P stars. No major differences in heavier elements between 1P and 2P. | Medium composed of pure ejecta from p-capture processes associated with multiple-population polluters. |
| 2P (middle stream) | Intermediate levels of C, N, O, Na, and Al between upper-stream 2P and 1P stars. Li, Mg, and Si are consistent with 1P abundances. | Result of dilution between pure 2P ejecta and a primordial, 1P-like medium. |
| AII (upper stream) | Light-element patterns similar to those in AI stars compared to 1P–2P differences. Covers a broad [Fe/H] range. N, O, Na, Mg, Al, s-process elements, and C+N+O increase with [Fe/H]; Si decreases. | Formed from a mixture of polluters: p-capture ejecta from AI stars, 3–4M⊙ AGB stars, and SN Ia. Higher [Fe/H] stars result from material ejected by iron-richer sources. |
| AII (middle stream) | Light-element abundances are intermediate between upper-stream AII and AI stars, similar to middle-stream 2P stars. Shows a smaller iron spread than anomalous stars in the upper and lower streams. [Fe/H] decreases toward the lower stream. | Originates from dilution between upper-stream AII-like gas and lower-stream-like material with lower average [Fe/H]. |
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