dc.creator | Lian, Jianhui | |
dc.creator | Zasowski, Gail | |
dc.creator | Hasselquist, Sten | |
dc.creator | Holtzman, Jon A | |
dc.creator | Boardman, Nicholas | |
dc.creator | Cunha, Katia | |
dc.creator | Fernández-Trincado, José G | |
dc.creator | Frinchaboy, Peter M | |
dc.creator | Garcia-Hernandez, D A | |
dc.creator | Nitschelm, Christian | |
dc.creator | Lane, Richard R | |
dc.creator | Thomas, Daniel | |
dc.creator | Zhang, Kai | |
dc.date.accessioned | 2023-02-27T15:56:10Z | |
dc.date.available | 2023-02-27T15:56:10Z | |
dc.date.issued | 2022 | |
dc.identifier.uri | https://doi.org/10.1093/mnras/stac479 | |
dc.identifier.uri | https://repository.tcu.edu/handle/116099117/57367 | |
dc.description.abstract | Stellar 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 rbirth < 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.language | en | |
dc.publisher | Oxford University Press (OUP) | |
dc.source | Monthly Notices of the Royal Astronomical Society | |
dc.subject | Space and Planetary Science | |
dc.subject | Astronomy and Astrophysics | |
dc.title | Quantifying radial migration in the Milky Way: inefficient over short time-scales but essential to the very outer disc beyond ~15 kpc | |
dc.type | Article | |
dc.rights.license | CC BY 4.0 | |
local.college | College of Science and Engineering | |
local.department | Physics and Astronomy | |
local.persons | Frinchaboy (PHYS) | |