# The Brightest Galaxies at Cosmic Dawn from Scatter in the Galaxy Luminosity versus Halo Mass Relation

## TL;DR

This paper models the ultraviolet luminosity function of galaxies at high redshift, showing how scatter and feedback processes influence the bright end shape and making predictions for future surveys to better understand early galaxy formation.

## Contribution

It introduces a semi-empirical model incorporating luminosity scatter to explain the UVLF shape at high redshift, highlighting the role of feedback and stochasticity in galaxy luminosity evolution.

## Key findings

- Scatter broadens the bright end of the UVLF at z>6.
- Feedback mechanisms shape the UVLF, either by a feedback scale or a luminosity threshold.
- Predictions for future surveys like WFIRST to constrain feedback and star formation processes.

## Abstract

The Ultraviolet Luminosity Function (UVLF) is a key observable for understanding galaxy formation from cosmic dawn. There has been considerable debate on whether Schechter-like LFs (characterized by an exponential drop-off at the bright end) that well describe the LF in our local Universe are also a sufficient description of the LF at high redshifts ($z>6$). We model the UVLF over cosmic history with a semi-empirical framework and include a log-normal scatter, $\Sigma$, in galaxy luminosities with a conditional luminosity function approach. We show that stochasticity induces a flattening or a feedback scale in the median galaxy luminosity versus halo mass relation, $L_{c}(M_{h})$ to account for the increase of bright objects placed in lower mass halos. We observe a natural broadening in the bright-end exponential segment of the UVLF for $z>6$ if processes that regulate star-formation acts on the same mass scale as at $z\sim5$, where the degree of broadening is enhanced for larger $\Sigma$. Alternatively, if the bright-end feedback is triggered at a near-constant luminosity threshold, the feedback threshold occurs at progressively lower halo masses with increasing redshift, due to galaxies being more luminous on average at a fixed halo mass from rapid halo assembly. Such feedback results in a LF shape with a bright-end closer to that of a Schechter function. We include predictions for the $z>8$ UVLFs from future all-sky surveys such as WFIRST which has the potential to both quantify the scatter and type of feedback, and provide insight behind the mechanisms that drive star formation in the early Universe.