Fig. 4.
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Non-LTE abundance correction for A(Ti)Ti I and A(Ti)Ti II, averaged over lines, as a function of Teff for the GALAH sample. The trends for dwarfs and giants are shown as solid and dashed lines, respectively, using bins of ΔTeff = ±75 K and limited to bins containing at least 30 stars. The colour gradient represents the number of stars per pixel.
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