Primordial Gas Collapse in The Presence of Radiation: Direct Collapse Black Hole or Population III star?

TL;DR

This paper investigates how the radiation spectrum from early galaxies influences whether primordial gas collapses into Population III stars or massive black holes, impacting early universe structure formation.

Contribution

It analyzes the role of radiation spectrum in primordial gas collapse, distinguishing conditions leading to star formation versus black hole formation.

Findings

Radiation spectrum determines the cooling pathway of primordial gas.

Lyman-Werner photons dissociate molecular hydrogen, affecting star or black hole formation.

Spectrum influences whether gas forms Pop. III stars or direct collapse black holes.

Abstract

The first billion years in the evolution of the Universe mark the formation of the first stars, black holes and galaxies. The radiation from the first galaxies plays an important role in determining the final state of primordial gas collapsing in a neighboring halo. This is due to the fact that the primary coolant for primordial gas is molecular hydrogen, which can be dissociated into atomic hydrogen by Lyman-Werner photons in the energy range $11.2 - 13.6$~eV. While cooling by molecular hydrogen leads to Pop. III star formation, cooling by atomic hydrogen can lead to the formation of a supermassive star (or quasi-star) which results in the formation of a massive $10^{4-5} M_\odot$ black hole, or a direct collapse black hole. The spectrum of this radiation field is critical in order to determine whether a primordial gas cloud forms a Pop. III star or a very massive black hole. We will in the following explore this scenario and discuss how the radiation spectrum influences the outcome of the collapse.