Density modulated star formation efficiency: implications for the observed abundance of ultra-violet luminous galaxies at z>10

TL;DR

This paper introduces a density-dependent star formation efficiency model into galaxy formation simulations, successfully explaining the high abundance and slow decline of ultra-violet luminous galaxies at redshifts greater than 10.

Contribution

It presents a novel density-modulated star formation efficiency model integrated into semi-analytic galaxy formation simulations, aligning predictions with high-redshift galaxy observations.

Findings

Models with density-modulated SFE match observed galaxy densities at z~6-17.

Increased bursty star formation and reduced dust attenuation explain early galaxy abundance.

Effective gas density dependence may vary with cosmic time, improving model fit.

Abstract

The number density of UV luminous galaxies discovered by the James Webb Space Telescope at ultra high redshift ($z \gtrsim 10$) is higher, and declines much more slowly with increasing redshift, than expected from extrapolations of lower redshift observations or pre-launch physics-based models. Most of these models assume star formation efficiencies (SFE) of only a few percent, motivated by observations of nearby galaxies. In this work, we incorporate a scaling of SFE with gas surface density (which we refer to as Density Modulated SFE; DMSFE), motivated by cloud-scale simulations and theory, into a semi-analytic cosmological model (SAM) of galaxy formation which is calibrated to match the observed rest-UV sizes of high redshift galaxies. We also model the impact of dust and bursty star formation on the SAM-predicted properties of observed galaxies. We show that with plausible values of the main parameters, such as the fraction of gas in dense clouds $f_{\rm dense}$, our new models easily reproduce or even exceed the observed galaxy number densities at $z\sim 6$-17. While no single value of $f_{\rm dense}$ is able to reproduce the very shallow observed decline of the galaxy number density at $z\gtrsim 12$, it is plausible and even expected for $f_{\rm dense}$ to have some effective dependence on cosmic time, which could bring these models into closer agreement with the data. We show that the combined effects of DMSFE, decreasing dust attenuation, and increasingly bursty star formation at earlier cosmic epochs could conspire to reproduce the observed evolution.