Quantifying radial migration in the Milky Way: inefficient over short time-scales but essential to the very outer disc beyond ∼15 kpc

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dc.contributor.authorLian, Jianhui
dc.contributor.authorZasowski, Gail
dc.contributor.authorHasselquist, Sten
dc.contributor.authorHoltzman, Jon A.
dc.contributor.authorBoardman, Nicholas
dc.contributor.authorCunha, Katia
dc.contributor.authorFernandez-Trincado, Jose G.
dc.contributor.authorFrinchaboy, Peter M.
dc.contributor.authorGarcia-Hernandez, D. A.
dc.contributor.authorNitschelm, Christian
dc.contributor.authorLane, Richard R.
dc.contributor.authorThomas, Daniel
dc.contributor.authorZhang, Kai
dc.date.accessioned2025-01-20T21:11:42Z
dc.date.available2025-01-20T21:11:42Z
dc.date.issued2022
dc.description.abstractStellar radial migration plays an important role in reshaping a galaxy's structure and the radial distribution of stellar population properties. In this work, we revisit reported observational evidence for radial migration and quantify its strength using the age-[Fe/H] distribution of stars across the Milky Way with APOGEE data. We find a broken age-[Fe/H] relation in the Galactic disc at r > 6 kpc, with a more pronounced break at larger radii. To quantify the strength of radial migration, we assume stars born at each radius have a unique age and metallicity, and then decompose the metallicity distribution function (MDF) of mono-age young populations into different Gaussian components that originated from various birth radii at r(birth) < 13 kpc. We find that, at ages of 2 and 3 Gyr, roughly half the stars were formed within 1 kpc of their present radius, and very few stars (<5 per cent) were formed more than 4 kpc away from their present radius. These results suggest limited short-distance radial migration and inefficient long-distance migration in the Milky Way during the last 3 Gyr. In the very outer disc beyond 15 kpc, the observed age-[Fe/H] distribution is consistent with the prediction of pure radial migration from smaller radii, suggesting a migration origin of the very outer disc. We also estimate intrinsic metallicity gradients at ages of 2 and 3 Gyr of -0.061 and -0.063 dex kpc(-1), respectively.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stac479
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stac479
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93630
dc.identifier.wosidWOS:000766832400003
dc.issue.numero4
dc.language.isoen
dc.pagina.final5655
dc.pagina.inicio5639
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectGalaxy: abundances
dc.subjectGalaxy: evolution
dc.subjectGalaxy: formation
dc.subjectGalaxy: stellar content
dc.subjectGalaxy: structure
dc.titleQuantifying radial migration in the Milky Way: inefficient over short time-scales but essential to the very outer disc beyond ∼15 kpc
dc.typeartículo
dc.volumen511
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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