A fundamental test for stellar feedback recipes in galaxy simulations. Issue 2 (6th March 2019)

• Record Type: Journal Article
• Authors: Fujimoto, Yusuke; Chevance, Mélanie; Haydon, Daniel T; Krumholz, Mark R; Kruijssen, J M Diederik
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 487:Issue 2(2019)
• Page Start: 1717
• Page End: 1728
• Publication Date: 2019-03-06
• Subjects: hydrodynamics -- methods: numerical -- ISM: clouds -- ISM: kinematics and dynamics -- galaxies: evolution -- galaxies: ISM; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz641
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Direct comparisons between galaxy simulations and observations that both reach scales ≲100 pc are strong tools to investigate the cloud-scale physics of star formation and feedback in nearby galaxies. Here we carry out such a comparison for hydrodynamical simulations of a Milky Way-like galaxy, including stochastic star formation, $\mathrm{H}\, {\small II}$ region and supernova feedback, and chemical post-processing at 8 pc resolution. Our simulation shows excellent agreement with almost all kpc-scale and larger observables, including total star formation rates, radial profiles of CO, H i, and star formation through the galactic disc, mass ratios of the ISM components, both whole galaxy and resolved Kennicutt–Schmidt relations, and giant molecular cloud properties. However, we find that our simulation does not reproduce the observed decorrelation between tracers of gas and star formation on ≲100 pc scales, known as the star formation 'uncertainty principle', which indicates that observed clouds undergo rapid evolutionary life cycles. We conclude that the discrepancy is driven by insufficiently strong pre-supernova feedback in our simulation, which does not disperse the surrounding gas completely, leaving star formation tracer emission too strongly associated with molecular gas tracer emission, inconsistent with observations. This result implies that the cloud-scale decorrelation of gas and star formation is a fundamental test for feedback prescriptions in galaxy simulations, one that can fail even in simulations that reproduce all other macroscopic properties of star-forming galaxies.