The chemical DNA of the Magellanic Clouds VI. Origin and evolution of neutron-capture elements in the SMC

TL;DR

This paper models the chemical evolution of the Small Magellanic Cloud, focusing on neutron-capture elements, and successfully reproduces observed abundance patterns by incorporating specific nucleosynthetic contributions and a top-lighter IMF.

Contribution

It introduces detailed chemical evolution models for the SMC that include neutron-capture elements and tests these models against recent observations, providing new insights into dwarf galaxy evolution.

Findings

Models reproduce observed abundance patterns of neutron-capture elements.

Enhanced r-process contribution and top-lighter IMF are necessary for matching data.

Provides first detailed evolution of multiple n-capture elements in a dwarf galaxy.

Abstract

Context. In the context of galactic archaeology, the study of the Small Magellanic Cloud (SMC) is of crucial importance, as it represents a unique opportunity to study a nearby massive dwarf system. However, theoretical studies of the chemical evolution of this galaxy are strikingly lacking. Aims. In this study, we investigate the chemical enrichment of the SMC galaxy. Besides alpha and Fe-peak elements, we devote particular attention to the evolution of neutron-capture elements with different origin, namely r-process (Eu), weak s-process (Zr) and main s-process (Ba, La). Methods. We develop chemical evolution models that use as input the star formation histories obtained from colour-magnitude diagram fitting. We follow in detail the chemical feedback provided by a large variety of nucleosynthetic sources. Model predictions are compared with recent abundance measurements for the SMC. Results. The developed framework reproduces well all the observables for elements up to the Fe-peak. The abundance patterns of n-capture elements are simultaneously reproduced only by assuming an enhanced contribution from the delayed r-process at low metallicity and a top-lighter IMF relative to the reference IMF by Kroupa (2001). In this way, both the observed very high plateau in [Eu/Fe] and the rising trends in [s-process/Fe] ratios can be reproduced by the models. Conclusions. This study provides for the first time information on the evolution of several n-capture elements in a massive dwarf irregular galaxy, also providing insight on several ingredients driving galactic evolution. Moreover, this work provides a test-bed for further modelling of the SMC in the context of the numerous surveys that will target the Magellanic Clouds in the next years.