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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 3.

Panels (a) and (b): distribution of the abundance ratios [Na/Fe] and [Mg/Fe], as a function of [Fe/H]. Panels (c) and (d): the same ratios, as a function of A(C). The open green triangles and orange circles represent Group II and Group III stars, respectively. The filled green and orange stars are the well-studied CEMP-no stars BD+44 493 and HE 1327-2326, which we take as type examples of Group II and Group III CEMP-no stars, respectively. Note that only stars with available classifications, based on the [Ba/Fe] criterion, are shown. A typical observational error bar is shown in the bottom left of each panel.

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