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The present-day Age-Metallicity Relation (AMR) is a record of the starformation history of the Galaxy, as this traces the chemical enrichment of thegas over time. We use a zoomed-in cosmological simulation that reproduces keysignatures of the Milky Way (MW), g2.79e12 from the NIHAO-UHD project, toexamine how stellar migration and satellite infall shape the AMR across thedisk. We find in the simulation, similar to the MW, the AMR in small spatialregions (R, z) shows turning points that connect changes in the direction ofthe relations. The turning points in the AMR in the simulation, are a signatureof late satellite infall. This satellite infall has a mass radio similar asthat of the Sagittarius dwarf to the MW (~ 0.001). Stars in the apex of theturning points are young and have nearly not migrated. The late satelliteinfall creates the turning points via depositing metal-poor gas in the disk,triggering star formation of stars in a narrow metallicity range compared tothe overall AMR. The main effect of radial migration on the AMR turning pointsis to widen the metallicity range of the apex. This can happen when radialmigration brings stars born from the infallen gas in other spatial bins, withslightly different metallicities, into the spatial bin of interest. Theseresults indicate that it is possible that the passage of the Sagittarius dwarfgalaxy played a role in creating the turning points that we see in the AMR inthe Milky Way.

Turning Points in the Age-Metallicity Relations -- Created by Late Satellite Infall and Enhanced by Radial Migration