The Stellar Populations of M33's Outer Regions

We have modelled the observed colour–magnitude diagram (CMD) at one location in M33’s outskirts under the framework of a simple chemical evolution scenario which adopts instantaneous and delayed recycling for the nucleosynthetic products of Type II and Ia supernovae. In this scenario, interstellar gas forms stars at a rate modulated by the Kennicutt–Schmidt relation and gas outflow occurs at a rate proportional to the star formation rate (SFR). With this approach, we put broad constraints on the role of gas flows during this region’s evolution and compare its [α/Fe] versus [Fe/H] relation with that of other Local Group systems. We find that models with gas inflow are significantly better than the closed-box model at reproducing the observed distribution of stars in the CMD. The best models have a majority of gas inflow taking place in the last 7 Gyr, and relatively little in the last 3 Gyr. These models predict most stars in this region to have [α/Fe] ratios lower than the bulk of the Milky Way’s halo. The predictions for the present-day SFR, gas mass and oxygen abundance compare favourably to independent empirical estimates. Our results paint a picture in which M33’s outer disc formed from the protracted inflow of gas over several Gyr with at least half of the total inflow occurring since z ∼ 1.