The Cosmic Evolution of the IMF Under the Jeans Conjecture with Implications for Bottom-Heavy Ellipticals

TL;DR

This paper models the evolution of the stellar initial mass function (IMF) in galaxies, showing it varies with the Jeans mass influenced by ISM conditions, affecting the mass-to-light ratio and aligning with some observational data.

Contribution

It introduces a model linking the IMF variation to the Jeans mass driven by ISM conditions, incorporating galaxy evolution and star formation histories.

Findings

IMF varies between top-heavy and bottom-heavy phases during galaxy evolution.

Mass-to-light ratios in massive galaxies are affected by early top-heavy IMFs.

Model aligns qualitatively with observed M/L ratios but may not explain all bottom-heavy features.

Abstract

We examine the cosmic evolution of a stellar initial mass function (IMF) in galaxies that varies with the Jeans mass in the interstellar medium, paying particular attention to the K-band stellar mass to light ratio (M/L_K) of present-epoch massive galaxies. We calculate the typical Jeans mass using high-resolution hydrodynamic simulations coupled with a fully radiative model for the ISM, which yields a parameterisation of the IMF characteristic mass as a function of galaxy star formation rate (SFR). We then calculate the star formation histories of galaxies utilising an equilibrium galaxy growth model coupled with constraints on the star formation histories set by abundance matching models. We find that at early times, energetic coupling between dust and gas drive warm conditions in the ISM, yielding bottom-light/top- heavy IMFs associated with large ISM Jeans masses for massive star-forming galaxies. Owing to the remnants of massive stars that formed during the top-heavy phases at early times, the resultant M/L_K(sigma) in massive galaxies at the present epoch is increased relative to the non- varying IMF case. At late times, lower cosmic ray fluxes allow for cooler ISM temperatures in massive galaxies, and hence newly formed clusters will exhibit bottom-heavy IMFs, further increasing M/L_K(sigma). Our central result is hence that a given massive galaxy may go through both top-heavy and bottom-heavy IMF phases during its lifetime, though the bulk of the stars form during a top-heavy phase. Qualitatively, the variations in M/L_K(sigma) with galaxy mass are in agreement with observations, however, our model may not be able to account for bottom-heavy mass functions as indicated by stellar absorption features.