A Multi-messenger Study of the Cygnus bubble
Abstract
We perform a comprehensive investigation of particle acceleration at the termination shocks of massive star clusters, with a particular focus on the Cygnus region. Building on the particle-acceleration model for cluster-driven winds, we use recently available spectral and spatial measurements of ultra-high-energy γ-rays from the Cygnus bubble to place stringent constraints on the physical conditions in the acceleration zone. By jointly modelling the observed γ-ray spectrum and spatial morphology, we derive quantitative limits on key parameters such as the maximum particle energy, acceleration efficiency, magnetic-field strength, and shock geometry, and assess their consistency with a hadronic origin of the emission. These data allow us to refine the target gas profiles within and around the bubble, thereby improving estimates of the expected hadronic γ-ray and neutrino fluxes. Using this revised gas model, we compute the neutrino emission associated with the Cygnus bubble and evaluate the statistical significance of a potential neutrino signal from this region for current and near-future high-energy neutrino observatories. Taken together, these results provide a more precise characterisation of the particle-acceleration environment at cluster termination shocks and help clarify the role of young massive star clusters as potential Galactic PeVatrons and contributors to the observed diffuse high-energy neutrino and γ-ray emissions.
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BibTeX
@misc{roy2026multimessenger,
title = {{A Multi-messenger Study of the Cygnus bubble}},
author = {Abhijit Roy and Giovanni Morlino and C Rishi and Jagdish C. Joshi and Soebur Razzaque and Neelam Panwar},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.03248},
eprint = {2611.03248},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.03248},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - A Multi-messenger Study of the Cygnus bubble
AU - Abhijit Roy
AU - Giovanni Morlino
AU - C Rishi
AU - Jagdish C. Joshi
AU - Soebur Razzaque
AU - Neelam Panwar
PY - 2026
DA - 2026/11/02
PB - arXiv
DO - 10.48550/arxiv.2611.03248
UR - https://arxiv.org/abs/2611.03248
AB - We perform a comprehensive investigation of particle acceleration at the termination shocks of massive star clusters, with a particular focus on the Cygnus region. Building on the particle-acceleration model for cluster-driven winds, we use recently available spectral and spatial measurements of ultra-high-energy γ-rays from the Cygnus bubble to place stringent constraints on the physical conditions in the acceleration zone. By jointly modelling the observed γ-ray spectrum and spatial morphology, we derive quantitative limits on key parameters such as the maximum particle energy, acceleration efficiency, magnetic-field strength, and shock geometry, and assess their consistency with a hadronic origin of the emission. These data allow us to refine the target gas profiles within and around the bubble, thereby improving estimates of the expected hadronic γ-ray and neutrino fluxes. Using this revised gas model, we compute the neutrino emission associated with the Cygnus bubble and evaluate the statistical significance of a potential neutrino signal from this region for current and near-future high-energy neutrino observatories. Taken together, these results provide a more precise characterisation of the particle-acceleration environment at cluster termination shocks and help clarify the role of young massive star clusters as potential Galactic PeVatrons and contributors to the observed diffuse high-energy neutrino and γ-ray emissions.
ER -