Available elemental abundances from de Castro et al. (2016) and Roriz et al. (2021a,b) and a selection of AGB models. Top panel: comparison of the abundance pattern of HD 154430 and the final surface abundances of different AGB models after applying dilution. The residuals for each model are shown in the bottom panel. The label box lists the mass of the current Ba star (M_Ba), the estimated initial mass of the AGB component () from Jorissen et al. (2019), and the parameters of the plotted models. All the masses are given in M_⊙ units. Specific properties of the FRUITY models are given in parentheses after the mass of each model: ‘---’ indicates the standard models, while ‘TAIL’, ‘rotating’, and ‘rotating TAIL’ models with 60 km s⁻¹ initial rotational velocity are indicated by (ext), (rNN), and (T60), respectively, where NN is the initial rotational velocity in km s⁻¹. The numbers given in parentheses after the mass of each Monash model represent the M_PMZ given in units of 10⁻⁴ M_⊙.