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Recent analysis of the SDSS-III/APOGEE Data Release 12 stellar catalogue hasrevealed that the Milky Way's metallicity distribution function (MDF) changesshape as a function of radius, transitioning from being negatively skewed atsmall Galactocentric radii to positively skewed at large Galactocentric radii.Using a high resolution, N-body+SPH simulation, we show that the changingskewness arises from radial migration - metal-rich stars form in the inner diskand subsequently migrate to the metal-poorer outer disk. These migrated starsrepresent a large fraction (> 50%) of the stars in the outer disk; theypopulate the high metallicity tail of the MDFs and are, in general, moremetal-rich than the surrounding outer disk gas. The simulation also reproducesanother surprising APOGEE result: the spatially invariant high-[alpha/Fe] MDFs.This arises in the simulation from the migration of a population formed withina narrow range of radii (3.2+/-1.2 kpc) and time (8.8+/-0.6 Gyr ago), ratherthan from spatially extended star formation in a homogeneous medium at earlytimes. These results point toward the crucial role radial migration has playedin shaping our Milky Way.

Imprints of radial migration on the Milky Way's metallicity distribution functions