Search for enhanced TeV gamma-ray emission from Giant Molecular Clouds using H.E.S.S
A. Sinha, V. Baghmanyan, G. Peron, Y. Gallant, S. Casanova, M. Holler,, A. Mitchell (for the H.E.S.S. collaboration)

TL;DR
This study uses 16 years of H.E.S.S. data and a 3D likelihood method to search for enhanced TeV gamma-ray emission from Giant Molecular Clouds, aiming to understand cosmic ray distribution in our Galaxy.
Contribution
It introduces a novel 3D likelihood analysis technique to differentiate gamma-ray emission from GMCs from background and diffuse emission in H.E.S.S. data.
Findings
No significant excess emission detected from GMCs.
Method effectively models background and diffuse emission.
Provides constraints on cosmic ray density variations.
Abstract
Cosmic Ray (CR) interactions with the dense gas inside Giant Molecular Clouds (GMCs) produce neutral pions, which in turn decay into gamma rays. Thus, the gamma ray emission from GMCs is a direct tracer of the cosmic ray density and the matter density inside the clouds. Detection of enhanced TeV emission from GMCs, i.e., an emission significantly larger than what is expected from the average Galactic cosmic rays illuminating the cloud, can imply a variation in the local cosmic ray density, due to, for example, the presence of a recent accelerator in proximity to the cloud. Such gamma-ray observations can be crucial in probing the cosmic ray distribution across our Galaxy, but are complicated to perform with present generation Imaging Atmospheric Cherenkov Telescopes (IACTs). These studies require differentiating between the strong cosmic-ray induced background, the large scale diffuse…
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Taxonomy
TopicsAstrophysics and Cosmic Phenomena · Dark Matter and Cosmic Phenomena · Particle Detector Development and Performance
