Effects of the integrated galactic IMF on the chemical evolution of the solar neighbourhood

TL;DR

This study investigates how the integrated galactic initial mass function (IGIMF), which varies with star formation rate, influences the chemical evolution of the solar neighborhood, highlighting the impact of different cluster mass function slopes.

Contribution

The paper introduces a time-varying IGIMF model based on the cluster mass function and demonstrates its effects on chemical evolution compared to a standard constant IMF.

Findings

Lower beta values lead to flatter IGIMFs with more massive stars.

The IGIMF with beta ~2 best reproduces observed stellar mass functions.

Higher supernova rates and gas ejection are associated with flatter IMFs.

Abstract

The initial mass function determines the fraction of stars of different intial mass born per stellar generation. In this paper, we test the effects of the integrated galactic initial mass function (IGIMF) on the chemical evolution of the solar neighbourhood. The IGIMF (Weidner & Kroupa 2005) is computed from the combination of the stellar intial mass function (IMF), i.e. the mass function of single star clusters, and the embedded cluster mass function, i.e. a power law with index beta. By taking into account also the fact that the maximum achievable stellar mass is a function of the total mass of the cluster, the IGIMF becomes a time-varying IMF which depends on the star formation rate. We applied this formalism to a chemical evolution model for the solar neighbourhood and compared the results obtained by assuming three possible values for beta with the results obtained by means of a standard, well-tested, constant IMF. In general, a lower absolute value of beta implies a flatter IGIMF, hence a larger number of massive stars and larger metal ejection rates. This translates into higher type Ia and II supernova rates, higher mass ejection rates from massive stars and a larger amount of gas available for star formation, coupled with lower present-day stellar mass densities. (abridged) We also discuss the importance of the present day stellar mass function (PDMF) in providing a way to disentangle among various assumptions for beta. Our results indicate that the model adopting the IGIMF computed with beta ~2 should be considered the best since it allows us to reproduce the observed PDMF and to account for most of the chemical evolution constraints considered in this work.