Constraining the near-IR background light from Population-III stars using high redshift gamma-ray sources

TL;DR

This paper uses high-redshift gamma-ray observations to constrain the contribution of Population-III stars to the near-infrared background light, providing limits on early star formation and the total background flux.

Contribution

It introduces a method to limit Population-III star formation rates using gamma-ray data and models their impact on the extragalactic background light.

Findings

Population-III star formation rate density is less than 0.5 M_solar yr^-1 Mpc^-3 at z=6-10.

Total background flux from Population-III stars is much less than that from resolved galaxies below 1.5 microns.

Current gamma-ray data can effectively constrain early star formation and background light contributions.

Abstract

The Fermi satellite has detected GeV emission from a number of gamma-ray bursts and active galactic nuclei at high redshift, z > 1.5. We examine the constraints that the detections of gamma rays from several of these sources place on the contribution of population-III stars to the extragalactic background light. Emission from these primordial stars, particularly redshifted Lyman-alpha emission, can interact with gamma rays to produce electron-positron pairs and create an optical depth to the propagation of gamma-ray emission, and the detection of emission above 10 GeV can therefore constrain the production of this background. We consider two initial mass functions for the early stars, and use derived SEDs for each to put upper limits on the star-formation rate density of massive early stars from redshifts 6 to 10. Our limits are complementary to those set on a high near-IR background flux by ground-based TeV-scale observations, and show that current data can limit star-formation in the late stages of reionization to less than 0.5 M_solar yr^-1 Mpc^-3. Our results also show that the total background flux from population-III stars must be considerably less than that from resolved galaxies at wavelengths below 1.5 microns.