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OBSERVATIONAL CONSTRAINTS ON FIRST-STAR NUCLEOSYNTHESIS. I. EVIDENCE FOR MULTIPLE PROGENITORS OF CEMP-NO STARS

  • Authors: Jinmi Yoon, Timothy C. Beers, Vinicius M. Placco, Kaitlin C. Rasmussen, Daniela Carollo, Siyu He, Terese T. Hansen, Ian U. Roederer, and Jeff Zeanah

2016 The Astrophysical Journal 833 20.

  • Provider: AAS Journals

Caption: Figure 7.

Comparison between stars sub-classified into the CEMP-s/rs and CEMP-no categories using either the [Ba/Fe] or the A(C) criterion. As before, the blue and red colors indicate the CEMP-s/rs and CEMP-no stars, respectively. The left panels correspond to use of the [Ba/Fe] criterion, while the right panels are based on the A(C) criterion. That is, CEMP-no stars are classified as such if they have A(C) ≤ 7.1, while CEMP-s/rs stars are classified as such if they have A(C) > 7.1. There are 15 stars with upper limits on [Ba/Fe] < 0.0 not shown in this figure. A typical observational error bar is shown in the bottom left of each panel.

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