From giant clumps to clouds I: the impact of gas fraction evolution on the stability of galactic discs

TL;DR

This study uses simulations to explore how varying gas fractions influence the stability and morphology of galactic discs, revealing a transition from clumpy to spiral structures as gas content decreases.

Contribution

It demonstrates how gas fraction evolution affects disc stability regimes and the formation of giant clumps versus spiral structures in galaxies.

Findings

Low gas fraction discs lack small-scale instabilities.

Gas-rich galaxies show significant molecular gas influence.

Transition at ~20% gas fraction marks the end of clumpy phase.

Abstract

The morphology of gas-rich disc galaxies at redshift ~1-3 is dominated by a few massive clumps. The process of formation or assembly of these clumps and their relation to molecular clouds in contemporary spiral galaxies are still unknown. Using simulations of isolated disc galaxies, we study how the structure of the interstellar medium and the stability regime of the discs change when varying the gas fraction. In all galaxies, the stellar component is the main driver of instabilities. However, the molecular gas plays a non-negligible role in the inter-clumps medium of gas-rich cases, and thus in the assembly of the massive clumps. At scales smaller than a few 100 pc, the Toomre-like disc instabilities are replaced by another regime, specially in the gas-rich galaxies. We find that galaxies at low gas fraction (10%) stand apart from discs with more gas, which all share similar properties on virtually all the aspects we explore. For gas fractions below approximately 20%, the clump-scale regime of instabilities disappears, only leaving the large-scale disc-driven regime. When translating the change of gas fraction to the cosmic evolution of galaxies, this transition marks the end of the clumpy phase of disc galaxies, and allows for the onset of spiral structures, as commonly found in the local Universe.