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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 6.

Distribution of [Fe/H], as a function of [Ba/Fe] (left panels), and [Ba/Fe], as a function of A(C) (right panels). As before, the blue and red colors indicate the CEMP-s/rs and CEMP-no stars, respectively. The gray shaded region in both panels represents stars with intermediate [Ba/Fe] ratios, 0.0 < [Ba/Fe] < +1.0, which complicates their sub-classification. The dashed vertical line in the right panel is a fiducial at A(C) = 7.1, placed between the peaks of the histograms of the A(C) distributions for Group I and Group II and III stars shown in Figure 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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