151. Unveiling the time evolution of chemical abundances across the Milky Way disk with APOGEE
- Author
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Ratcliffe, Bridget, Minchev, Ivan, Anders, Friedrich, Khoperskov, Sergey, Guiglion, Guillaume, Buck, Tobias, Cunha, Katia, Queiroz, Anna, Nitschelm, Christian, Meszaros, Szabolcs, Steinmetz, Matthias, de Jong, Roelof S., Nepal, Samir, Lane, Richard R., and Sobeck, Jennifer
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Chemical abundances are an essential tool in untangling the Milky Way's enrichment history. However, the evolution of the interstellar medium abundance gradient with cosmic time is lost as a result of radial mixing processes. For the first time, we quantify the evolution of many observational abundances across the Galactic disk as a function of lookback time and birth radius, $R_\text{birth}$. Using an empirical approach, we derive $R_\text{birth}$ estimates for 145,447 APOGEE DR17 red giant disk stars, based solely on their ages and [Fe/H]. We explore the detailed evolution of 6 abundances (Mg, Ca ($\alpha$), Mn (iron-peak), Al, C (light), Ce (s-process)) across the Milky Way disk using 87,426 APOGEE DR17 red giant stars. We discover that the interstellar medium had three fluctuations in the metallicity gradient $\sim 9$, $\sim 6$, and $\sim4$ Gyr ago. The first coincides with the end of high-$\alpha$ sequence formation around the time of the Gaia-Sausage-Enceladus disruption, while the others are likely related to passages of the Sagittarius dwarf galaxy. A clear distinction is found between present-day observed radial gradients with age and the evolution with lookback time for both [X/Fe] and [X/H], resulting from the significant flattening and inversion in old populations due to radial migration. We find the [Fe/H]--[$\alpha$/Fe] bimodality is also seen as a separation in the $R_\text{birth}$--[X/Fe] plane for the light and $\alpha$-elements. Our results recover the chemical enrichment of the Galactic disk over the past 12 Gyr, providing tight constraints on Galactic disk chemical evolution models., Comment: accepted for publication in MNRAS
- Published
- 2023
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