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Stellar radial migration plays an important role in reshaping a galaxy'sstructure and the radial distribution of stellar population properties. In thiswork, we revisit reported observational evidence for radial migration andquantify its strength using the age--[Fe/H] distribution of stars across theMilky Way with APOGEE data. We find a broken age--[Fe/H] relation in theGalactic disc at $r>6$ kpc, with a more pronounced break at larger radii. Toquantify the strength of radial migration, we assume stars born at each radiushave a unique age and metallicity, and then decompose the metallicitydistribution function (MDF) of mono-age young populations into differentGaussian components that originated from various birth radii at $r_{\rmbirth}<13$ kpc. We find that, at ages of 2 and 3 Gyr, roughly half the starswere formed within 1 kpc of their present radius, and very few stars ($<5$%)were formed more than 4 kpc away from their present radius. These resultssuggest limited short distance radial migration and inefficient long distancemigration in the Milky Way during the last 3 Gyr. In the very outer disc beyond15~kpc, the observed age--[Fe/H] distribution is consistent with the predictionof pure radial migration from smaller radii, suggesting a migration origin ofthe very outer disc. We also estimate intrinsic metallicity gradients at agesof 2 and 3 Gyr of $-0.061$ dex kpc$^{-1}$ and $-0.063$ dex kpc$^{-1}$,respectively.

Quantifying radial migration in the Milky Way: Inefficient over short timescales but essential to the very outer disc beyond ~15 kpc