Star formation histories of chemodynamical components in the Milky Way derived from MSTO ages at ﹩1\lesssim | Z| \lesssim 4\,\mathrm{kpc}﹩. The accreted halo (metal-poor stars on eccentric orbits; blue line) is older than the in situ halo (high-α stars on eccentric orbits; red line). The star formation history of the in situ halo is very similar to that of high-α stars on disk-like, circular orbits (red dotted line). The MSTO stars above the Galactic plane show that the low-α disk forms last (orange dotted line), although they are likely not representative of the global low-α population, which we expect continues forming stars at the present. The typical age uncertainty for a single star is ≈1 Gyr, shown with an error bar below the legend, so the detected difference in the distribution of ages between the in situ and the accreted halo is significant.