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Fig. 3

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Left: birth radii of stars ending up in the “solar” radius (green shaded strip) at the final simulation time. The solid black curve plots the total r0-distribution, while the color-coded curves show the distributions of stars in six different age groups, as indicated. The dotted-red and solid-blue vertical lines indicate the positions of the bar’s CR and OLR at the final simulation time. A large fraction of old stars comes from the inner disk, including from inside the CR. Middle: [Fe/H] distributions for stars ending up in the green-shaded strip (left) binned by birth radii in six groups, as indicated. The total distribution is shown by the solid black curve. The importance of the bar’s CR is seen in the large fraction of stars with 3 < r0 < 5 kpc (blue line). Right: density contours of the r0-[Fe/H] plane for local stars. The cyan curve shows our model solar-age metallicity gradient. Taking an error of ±1 dex in [Fe/H], we find a possible Sun birth radius of 4.6 < r0 < 7.6 kpc (where the horizontal green, transparent strip meets the cyan line). The imbedded histogram shows the density of stars in the likely r0-range, indicating a decline in the probability for r0 ≲ 5.5 kpc.

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