Correlated GeV-TeV Gamma-Ray Emission from Extended Sources in the Cygnus Region

TL;DR

This paper analyzes gamma-ray emissions from the Cygnus region using HAWC and Fermi-LAT data, revealing correlations across GeV to TeV energies and providing insights into the region's complex astrophysical sources.

Contribution

It presents a comprehensive multi-instrument analysis of gamma-ray sources in Cygnus, highlighting the correlation between GeV and TeV emissions and advancing understanding of their origins.

Findings

Detection of correlated GeV-TeV gamma-ray emission in Cygnus

Enhanced understanding of the morphology of gamma-ray sources

Insights into the emission mechanisms of the Cygnus Cocoon

Abstract

The Cygnus arm of our galaxy is a source-rich and complex region hosting multiple gamma-ray source types such as pulsar wind nebulae (PWN), supernova remnants, binary systems, and star clusters. The High Altitude Water Cherenkov (HAWC) observatory has been collecting data continuously since 2015 and has reported five sources within the Cygnus region. Several other instruments have also observed gamma-ray sources in this region. For instance, Fermi-LAT found gamma-ray emission at GeV energies due to a Cocoon of freshly accelerated cosmic rays, which is co-located with a known PWN TeV 2032+4130 seen by several TeV gamma-ray observatories. TeV J2032+4130 is likely powered by the pulsar PSR J2032+4127 based on the multi-wavelength observation and asymmetric morphology reported by VERITAS. The study of HAWC data will provide more information regarding the morphology, emission origin, and the correlation with the GeV emission. This presentation will discuss the analysis of data collected with the HAWC instrument and the Fermi-LAT and the results obtained to provide a deeper understanding of the Cygnus Cocoon across five decades of energy range.