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tokens: are quite discrepant (0.2 dex and 0.8 dex in our two stars, respectively). The 4215.5 Å line of the star S11–97 is affected by the CN molecular band in this region. Spectral synthesis taking into account the carbon abundance derived in the CH band led to an abundance that agrees better with the 4077.7 Å line. Yttrium. Two very faint lines ( 15 mÅ) of yttrium were detected in our spectra, but we were only able to place upper limits on the Y abundance in our stars. Barium. Four lines of barium are present in our wavelength ranges. One is very faint ( λ 5853 Å) and detected for only one star, and the other three lines are strong. Two of them are blended with weak iron lines ( λ 4934 Å and λ 6141 Å). Therefore we proceeded by spectral synthesis, taking into account all blends and the Ba HFS components. Barium has five isotopes; different fractions of even-A and odd-A (A=atomic mass) nuclei ( 134 Ba + 136 Ba + 138 Ba) : ( 135 Ba + 137 Ba) were tested: the 82:18 solar fraction, and the r -process fractions of 54:46 and 28:72. The Ba λ 4934 Å resonance line is more sensitive than the three subordinate lines to the adopted fraction. The solar 82:18 fraction led to the best agreement between the resonance and the subordinates lines. We refer to Jablonka et al. (2015) , Mashonkina et al. (2017b) for a more detailed investigation of the possible cause. 5. Discussion 5.1. Carbon Figure 3 shows that none of our stars can be considered as carbon-enhanced based on the Aoki et al. (2007) criterion. Nonetheless, our stars are evolved enough to have converted C into N by the CNO cycle, as they are above log( L ⋆ / L ⊙ ) = 2.3, that is, the limit above which a metal-poor 0.8 M ⊙ star is thought to undergo additional mixing between the bottom of the stellar convective envelope and the outer layer of the advancing hydrogen shell (see Placco et al. 2014 , and references therein for a discussion). Fig. 3. [C/Fe] as a function of log( L / L ⊙ ) for Galactic dwarf satellite and halo red giants with metallicities [Fe/H] –2.5. The Sextans stars we analyzed are represented by large red circles. Red squares are Sextans stars from Tafelmeyer et al. (2010) , the red triangle is the Sextans carbon-rich star from Honda et al. (2011) . Gray dots denote the [C/Fe] abundances of MW halo stars from Yong et al. (2013) . RGB stars in Sculptor ( Jablonka et al. 2015 ; Simon et al. 2015 ; Tafelmeyer et al. 2010 ), Fornax ( Tafelmeyer et al. 2010 ), and Draco ( Shetrone et al. 2013 ; Cohen Huang 2009 ) are shown in orange, blue, and green; respectively. The dotted line is the Aoki et al. (2007) dividing line for carbon enhancement, which takes into account the depletion of carbon with evolution along the RGB. Placco et al. (2014) developed a procedure for correcting the measured carbon abundances based on stellar model evolution and depending on the log(g) of the stars. They showed that when these corrections were applied to their dataset, the fraction of carbon-rich stars [C/Fe] >