# Size-scaling of clump instabilities in turbulent, feedback regulated disks

## TL;DR

This study investigates how the size of star-forming clumps in turbulent galactic disks scales with rotational support, using simulations and observations to test a theoretical relation under various feedback conditions.

## Contribution

It verifies the clump size scaling relation in observed and simulated galaxies and examines its robustness across different feedback models within the VDI framework.

## Key findings

- Clump size scaling relation holds for observed and simulated galaxies.
- Feedback processes influence the position of galaxies on the scaling relation.
- Large-scale instabilities are governed by Toomre-like stability criteria regardless of feedback.

## Abstract

We explore the scaling between the size of star-forming clumps and rotational support in massively star-forming galactic disks. The analysis relies on simulations of a clumpy galaxy at $z=2$ and the observed DYNAMO sample of rare clumpy analogs at $z\approx0.1$ to test a predictive clump size scaling proposed by \citet{Fisher2017ApJ...839L...5F} in the context of the Violent Disk Instability (VDI) theory. We here determine the clump sizes using a recently presented 2-point estimator, which is robust against resolution/noise effects, hierarchical clump substructure, clump-clump overlap and other galactic substructure. After verifying Fisher's clump scaling relation for the DYNAMO observations, we explore whether this relation remains characteristic of the VDI theory, even if realistic physical processes, such as local asymetries and stellar feedback, are included in the model. To this end, we rely on hydrodynamic zoom-simulations of a Milky Way-mass galaxy with four different feedback prescriptions. We find that, during its marginally stable epoch at $z=2$, this mock galaxy falls on the clump scaling relation, although its position on this relation depends on the feedback model. This finding implies that Toomre-like stability considerations approximately apply to large ($\sim\rm kpc$) instabilities in marginally stable turbulent disks, irrespective of the feedback model, but also emphasizes that the global clump distribution of a turbulent disk depends strongly on feedback.