Stellar Populations in a semi-analytic model I: bulges of Milky Way-like galaxies

TL;DR

This study uses a semi-analytic galaxy formation model to analyze the stellar populations of Milky Way-like galaxy bulges, revealing that most stars are accreted and formed during disc instability events, with implications for understanding bulge formation.

Contribution

The paper introduces a semi-analytic model adapted to trace properties of stellar populations in galaxy bulges, providing new insights into their formation processes and chemical compositions.

Findings

87% of bulge stars are accreted or formed in starbursts

Mergers account for 13% of bulge mass and influence metallicity

No observed gradient in [{}/Fe] ratios along the bulge minor axis

Abstract

We study the stellar populations of bulges of Milky Way-like (MW-like) galaxies with the aim of identifying the physical processes involved in the formation of the bulge of our Galaxy. We use the semi-analytic model of galaxy formation and evolution SAG adapted to this aim; this kind of models can trace the properties of galaxies and their components like stellar discs, bulges and halos, but resolution limits prevent them from reaching the scale of stellar populations (SPs). Properties of groups of stars formed during single star formation events are stored and tracked in the model and results are compared with observations of stars in the galactic bulge. MW-like galaxies are selected using two different criteria. One of them considers intrinsic photo-metric properties and the second is focused on the cosmological context of the local group of galaxies (LG). We compare our model results with spectroscopic and photometric stellar metallicity distributions. We find that 87% of stars in bulges of MWtype galaxies in our model are accreted and formed in starbursts during disc instability events. Mergers contribute to 13% of the mass budget of the bulge and are responsible for the low metallicity tail of the distribution. Abundance ratios of {\alpha} elements with respect to iron, [{\alpha}/Fe], are measured in SPs of model galaxies. The patterns found in the model for SPs with different origins help to explain the lack of a gradient of [{\alpha}/Fe] ratios in observed stars along the minor axis of the bulge.