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Fig. 7


[Sr/Ba] vs. [Ba/Fe] for i) our sample of EMP stars (Large Program First Stars restricted to the stars with −3.5 ≤ [ Fe/H ] ≤ −2.7), for ii) the CEMP stars in the same range of metallicity gathered from Aoki et al. (2001, 2002), Depagne et al. (2002), Barbuy et al. (2005), and Yong et al. (2013), and for iii) the three low-Sr/Ba giants (this paper). Symbols are the same as in Fig. 3. The three low-Sr/Ba giants occupy a very peculiar position in this diagram: they associate a low value of [Sr/Ba] like in the CEMP-s stars to a relatively low value of [Ba/Fe] ([ Ba/Fe ] < 1) like in the classical EMP stars or the CEMP-no.

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