YST and I realized that you can get really large metallicity gaps due to Type Ia SNe enrichment during long quiescent periods in a galaxy’s star formation history. The SNe keep going off even though you stop forming stars, which can show up in chemical evolution.

Ooh, that’s a great idea!

This type of model pushes the limits of current data, needing large numbers of precise abundances that will be possible in coming years with PFS/4MOST/ELTs. It’s also extremely powerful, providing unprecedented time resolution in low-mass dwarf galaxies inaccessible with direct observations.