Variations of the Initial Mass Function in Semi-Analytical models

TL;DR

This study explores how different assumptions about the evolving stellar initial mass function (IMF) affect galaxy property predictions in semi-analytical models, highlighting the importance of high-mass galaxy observations for constraining IMF variations.

Contribution

It systematically assesses the impact of various IMF evolution scenarios on galaxy properties within the MORGANA model, providing insights into how IMF variations influence galaxy formation predictions.

Findings

Top-Heavy IMF increases significantly affect galaxy properties.

Most IMF variations cause deviations within observational uncertainties.

High-mass galaxy studies can constrain IMF evolution models.

Abstract

Deviations from a universal, MW-like, Stellar Initial Mass Function (IMF) have been reported for distant galaxies, although the physical reason behind the observed variations is still matter of ongoing debate. In this paper, we present an exploratory study to assess the impact of the proposed IMF evolution on the statistical galaxy properties, as predicted by the Semi-Analytical model of galaxy formation and evolution MORGANA. In particular, we test different dependencies for the IMF shape, as a function of both model galaxy properties (such as star formation rate, velocity dispersion or stellar mass) and environment, and compare the predicted stellar mass functions and star formation rate functions with reference runs at fixed IMF. In most cases, MORGANA predictions show deviations of the order of a few tenths of dex with respect to a run assuming an Universal Kroupa IMF. Among the proposed IMF variations, an increasing Top-Heavy IMF at increasing star formation rates has the largest impact on predicted galaxy properties, while most of the models assuming an increasing Bottom-Heavy IMF at higher masses/velocity dispersion lead to variations in galaxy properties that are of the same order as the uncertainty on the mass and star formation rate determination. By comparing the predicted galaxy stellar mass functions, we conclude that the study of the high-mass end can provide useful constraints to disentangle models assuming an increasing Top-Heavy IMF in high star forming or Bottom-Heavy IMF in massive systems.