The Stellar Populations of M33's Outer Regions IV: Inflow History and Chemical Evolution

TL;DR

This study models the chemical evolution of M33's outer regions, showing that gas inflow over several billion years better explains observed stellar populations than closed models, with implications for galaxy formation.

Contribution

It introduces a chemical evolution model incorporating gas inflow and outflow, fitting observed CMD data and constraining inflow history in M33's outskirts.

Findings

Gas inflow models outperform closed box models.

Majority of gas inflow occurred in the last 7 Gyr.

Predicted [alpha/Fe] ratios are lower than Milky Way's halo.

Abstract

We have modelled the observed color-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 [alpha/Fe] vs. [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 [alpha/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 favorably 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.