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Title:
The stellar populations of M33's outer regions - IV. Inflow history and chemical evolution
Authors:
Barker, Michael K.; Sarajedini, A.
Affiliation:
AA(Department of Astronomy, University of Florida, Gainesville, FL 32611, USA; ), AB(Department of Astronomy, University of Florida, Gainesville, FL 32611, USA; )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 390, Issue 2, pp. 863-880. (MNRAS Homepage)
Publication Date:
10/2008
Origin:
MNRAS
MNRAS Keywords:
galaxies: abundances , galaxies: evolution , galaxies: individual: Messier Number: M33 , Local Group , galaxies: spiral , galaxies: stellar content
DOI:
10.1111/j.1365-2966.2008.13816.x
Bibliographic Code:
2008MNRAS.390..863B

Abstract

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.
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