Probing Galactic Diffuse TeV Gamma-Ray Emission with the HAWC Observatory

TL;DR

This paper discusses the methodology for detecting Galactic diffuse TeV gamma-ray emission using the HAWC Observatory, which can provide insights into cosmic-ray acceleration and propagation in our Galaxy.

Contribution

It introduces an analysis strategy with techniques to identify diffuse gamma-ray emission while removing contamination from localized sources.

Findings

Developed an analysis framework for diffuse emission detection.

Outlined methods to mitigate contamination from point sources.

Enhanced understanding of Galactic cosmic-ray interactions.

Abstract

Galactic diffuse TeV gamma-ray emission is produced by the interaction of high-energy cosmic-ray particles with matter and radiation in our Galaxy. The measurement of Galactic diffuse TeV gamma-ray emission would provide strong constraints on the acceleration and propagation of Galactic cosmic rays. The High Altitude Water Cherenkov (HAWC) Observatory, located in central Mexico at 4100 m above sea level, is sensitive to gamma rays between a few hundreds GeV and about 100 TeV. Thanks to its large field of view of 2 steradians and excellent background estimation, HAWC has a unique capability to observe large extended sources such as Galactic diffuse emission. We present the analysis strategy to detect the Galactic diffuse emission with HAWC, including techniques to remove contaminations from localized sources.