Analytical Modeling of Galaxies at z>~6: Star Formation and Black Hole Growth

TL;DR

This paper presents an analytical model for high-redshift galaxies (z>~6), linking their evolution to inflows, winds, and internal ISM physics, with implications for understanding galaxy formation and growth.

Contribution

It introduces a novel analytical framework combining inflow-wind balance and radiation pressure to explain galaxy properties at z>~6.

Findings

The UV mass-to-light ratio evolution from z~6--10 can be explained by inflow and wind dynamics.

Hydrostatic equilibrium and Toomre stability can be maintained by radiation pressure in dust-free disks.

X-ray observations can constrain the internal ISM physics of early galaxies.

Abstract

Galaxies at z>~6 represent an important evolutionary link between the first galaxies and their modern counterparts. Modeling both the global and internal properties of these recently discovered objects can lead us to understand how they relate to even earlier systems. I show how the balance of cold inflows and momentum-driven super-winds can explain the evolution of the UV mass-to-light ratio from z~6--10. I then describe a model for maintaining hydrostatic equilibrium and marginal Toomre-instability by radiation pressure in dust-free galactic disks. Applying this framework to z~6--8 systems, I show how the internal ISM physics can be constrained by X-rays observations with Chandra.