Fig. 7.

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Location of the AGBb in the plane log Teff; log νmax, in the mass bin, M ∈ [1.5, 2.5] M⊙, and metallicity bins, [Fe/H] ∈ [ − 1.0, −0.5], [ − 0.5, −0.25], [ − 0.25, 0.0], [0.0, 0.25] dex. The label is the same as in Fig. 5. An additional model represented by a black cross was computed to explore the effects of rotation by taking the rotation rate ΩZAMS/Ωcrit = 0.3 during the main sequence, relative to the reference model, where Ωcrit is the surface critical angular velocity for the star to be dislocated. Another model, labelled ‘test’ and represented by a black pentagon, was also computed to check if combining several changes could allow us to reproduce the observations. With respect to the reference model, these changes are the adding of rotation ΩZAMS/Ωcrit = 0.3, He-core overshooting αov, He = 1.0, the removal of H-core overshooting αov, H = 0.2 → 0, and the decrease of αMLT = 1.92 → 1.62. The numerical values are listed in Table A.4. We caution that the range of the axes are not the same between panels.
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