Exploring the Nature of the Galactic Center Gamma-Ray Source with the Cherenkov Telescope Array

TL;DR

This paper assesses the potential of the Cherenkov Telescope Array to distinguish between different gamma-ray emission models at the Galactic center, emphasizing CTA's high angular resolution in testing hadronic scenarios versus point sources or dark matter.

Contribution

It provides a detailed simulation-based evaluation of CTA's capability to detect extended gamma-ray emission and differentiate emission origins at the Galactic center.

Findings

CTA's angular resolution can conclusively test hadronic emission models.

Simulations show CTA can detect extended emission profiles.

Results inform dark matter search strategies in the Galactic center.

Abstract

Observations from multiple gamma-ray telescopes have uncovered a high energy gamma-ray source spatially coincident with the Galactic center. Recently, a compelling model for the broad-band gamma-ray emission has been formulated which posits that high energy protons emanating from Sgr A* could produce gamma-rays through pion decays resulting from inelastic collisions with the traversed interstellar gas in the region. Models of the gas distribution in the Galactic center region imply that the resulting gamma-ray morphology would be observed as a point source with all current telescopes, but that the upcoming Cherenkov Telescope Array (CTA) may be able to detect an extended emission profile with an unmistakable morphology. Here, we critically evaluate this claim, employing a three dimensional gas distribution model and a detailed Monte Carlo simulation, and using the anticipated effective area and angular resolution of CTA. We find that the impressive angular resolution of CTA will be key to test hadronic emission models conclusively against, for example, point source or dark matter annihilation scenarios. We comment on the relevance of this result for searches for dark matter annihilation in the Galactic center region.