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. 2023 Dec 23;527(4):12120–12139. doi: 10.1093/mnras/stad3973

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© 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

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Figure 9. — Evolutionary abundance trends of Mg, Ca, Ti, and Fe. Mg abundances are derived from neutral lines, while Ti and Fe are derived from lines of singly ionized species, and Ca is based on a mixture of lines of both neutral and singly ionized species. The trends are compared to predictions from stellar structure models including AD with AddMix with different efficiencies, at an age of 12 Gyr. Horizontal, dashed lines represent the initial abundances of the models, which have been adjusted so that predictions match the observed abundance level of the coolest stars. Blue squares represent results for group-averaged co-added spectra, while grey diamonds represent results for individual stars.