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Fig. 14.

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Inferred Rbirth versus true Rbirth for subhalo 560751 using the method from Lu et al. (2022a) with age and [Fe/H] uncertainties added of 15% and 0.05 dex respectively. Rbirth are estimated using the true evolution of [Fe/H](R = 0 kpc, τ) (black line in Fig. 13) and ∇[Fe/H](τ) recovered from Range [ Fe / H ] ( age ) $ \mathrm{Range}\widetilde{\mathrm{[Fe/H]}}\mathrm{(age)} $. The difference between the left and right panels is that stellar [Fe/H] values in the TNG50 galaxy were adapted to better match the dispersion about the metallicity gradient as seen in the Milky Way’s H II regions in the right panel. This illustrates the high probability of success in estimating Rbirth in the Milky Way disk.

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