Correlations between the abundances of Barium stars, the AGB model residuals and the delta parameter

<p>Additional figures for Vil&aacute;gos et al. 2024, Sect. 3.2. For the sample of Barium stars, correlations between the observationally dervied abundances; the residuals between the AGB models and the abundances; and the delta parameter.</p> <p>The figures are divided into the following directories:</p> <ul> <li>'1-obs_feh':&nbsp; Abundances and elemental ratios of different peaks as a function of the [Fe/H] (Sect. 3.2.1 and Fig. 5).</li> <li>'2-res_feh':&nbsp;&nbsp; Residuals of the abundances and elemental ratios as a function of the [Fe/H] (Sect. 3.2.2 and Fig. 6).</li> <li>'3-obs_obs': Abundances as a function of the other abundances (Sect. 3.2.3 and Fig. 7).</li> <li>'4-res_res':&nbsp;&nbsp; Residuals of the abundances as a function of the other residuals (Sect. 3.2.4 and Fig. 8).</li> <li>'5-res_obs':&nbsp; Residuals of the abundances as a function of the abundances (see Sect. 3.2.5 and Fig. 9).</li> <li>'6-delta':&nbsp;&nbsp;&nbsp;&nbsp;&nbsp;&nbsp; Abundances and residuals as a function of the delta parameter, that indicates the fraction of AGB material in the Ba star envelope (Sect. 3.2.6 and Fig. 10).</li> </ul> <p>For figures in directories 1-2, we refer to some elements as [A/B], although sometimes [B/A] vs. [Fe/H] is shown. Visually, this swapping of the numerator and denominator elements means a vertical reflection around the y = 0 axis. Thus, $r_S$ and $a$ for [B/A] vs. [Fe/H] have the same absolute value but different sign than for [A/B] vs. [Fe/H].</p> <p>For figures in directories 3-5, if we refer to [A/Fe] vs [B/Fe], but plot [B/Fe] vs [A/Fe], the sign of the relationship (correlation or anti-correlation) remains the same. The swap of the two axes results in a reflection around a diagonal line with a slope of 1. The resulting slope is therefore $1/a$, while $r_S$ is the same in both cases.</p>