Similarities behind the high- and low−α disk: small intrinsic abundance scatter and migrating stars

The detailed age-chemical abundance relations of stars measure time-dependent chemical evolution. These trends offer strong empirical constraints on nucleosynthetic processes, as well as the homogeneity of star-forming gas. Characterizing chemical abundances of stars across the Milky Way over time has been made possible very recently, thanks to surveys like Gaia, APOGEE and Kepler. Studies of the low-α disk have shown that individual elements have unique age-abundance trends and the intrinsic dispersion around these relations is small. In this study, we examine and compare the age distribution of stars across both the high and low-α disk and quantify the intrinsic dispersion of 16 elements around their age-abundance relations at [Fe/H] = 0 using APOGEE DR16. We examine the age-metallicity relation and visualize the temporal and spatial distribution of disk stars in small chemical cells. We find: 1) the high-α disk has shallower age-abundance relations compared to the low-α disk, but similar median intrinsic dispersions of ∼ 0.03 dex; 2) turnover points in the age-[Fe/H] relations across radius for both the high- and low-α disk. The former constrains the mechanisms that set similar intrinsic dispersions, regardless of differences in the enrichment history, for stars in both disks, and the latter indicates the presence of radial migration in both disks. Our study is accompanied by an age catalogue for 64,317 stars in APOGEE derived using The Cannon with a median uncertainty of 1.5 Gyr (26%) (APO-CAN stars), and a red clump catalogue of 22,031 stars with a contamination rate of 2.7%.