Calibrated, cosmological hydrodynamical simulations with variable IMFs I: method and effect on global galaxy scaling relations. Issue 4 (10th July 2018)

• Record Type: Journal Article
• Authors: Barber, Christopher; Crain, Robert A; Schaye, Joop
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 479:Issue 4(2018)
• Page Start: 5448
• Page End: 5473
• Publication Date: 2018-07-10
• Subjects: methods: numerical -- stars: luminosity function, mass function -- galaxies: elliptical and lenticular, cD -- galaxies: fundamental parameters -- galaxies: star formation -- galaxies: stellar content; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1826
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The recently inferred variations in the stellar initial mass function (IMF) among local high-mass early-type galaxies may require a reinterpretation of observations of galaxy populations and may have important consequences for the predictions of models of galaxy formation and evolution. We present a new pair of cosmological, hydrodynamical simulations based on the EAGLE model that self-consistently adopts an IMF that, respectively, becomes bottom- or top-heavy in high-pressure environments for individual star-forming gas particles. In such models, the excess stellar mass-to-light ( M/L ) ratio with respect to a reference IMF is increased due to an overabundance of low-mass dwarf stars or stellar remnants, respectively. Crucially, both pressure-dependent IMFs have been calibrated to reproduce the observed trends of increasing excess M/L with central stellar velocity dispersion (σe ) in early-type galaxies, while maintaining agreement with the observables used to calibrate the EAGLE model, namely the galaxy luminosity function, half-light radii of late-type galaxies, and black hole masses. We find that while the M/L excess is a good measure of the IMF for low-mass slope variations, it depends strongly on the age of the stellar population for high-mass slope variations. The normalization of the [Mg/Fe]−σe relation is decreased (increased) for bottom- (top-)heavy IMF variations, while the slope is not strongly affected. Bottom-heavy variations have little impact on galaxy metallicities, half-light radii of early-type galaxies, or star formation rates, while top-heavy variations significantly increase these quantities for high-mass galaxies, leading to tension with observations.