Deciphering the gamma-ray emission in the Cygnus region
The Cygnus region is a vast star-forming complex harbouring a population of powerful objects, including massive star clusters and associations, Wolf-Rayet stars, pulsars, and supernova remnants. The multi-wavelength picture is far from understood, particularly the recent LHAASO detection of multi-de...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
10 November 2025
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| In: |
Astronomy and astrophysics
Year: 2025, Jahrgang: 703 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202555531 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202555531 Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2025/11/aa55531-25/aa55531-25.html 
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| Verfasserangaben: | L. Härer, T. Vieu, F. Schulze, C.J.K. Larkin, and B. Reville |
MARC
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| 520 | |a The Cygnus region is a vast star-forming complex harbouring a population of powerful objects, including massive star clusters and associations, Wolf-Rayet stars, pulsars, and supernova remnants. The multi-wavelength picture is far from understood, particularly the recent LHAASO detection of multi-degree scale diffuse γ-ray emission up to PeV energies. We aim to model the broadband γ-ray data, discriminating plausible scenarios amongst all candidate accelerators. We consider in particular relic hadronic emission from a supernova remnant expanding in a low-density environment and inverse Compton emission from stellar-wind termination shocks in the Cygnus OB2 stellar association. We first estimated the maximum particle energy from a 3D hydrodynamical simulation of the supernova remnant scenario. The transport equation was then solved numerically to determine the radial distribution of non-thermal protons and electrons. In order to compute synthetic γ-ray spectra and emission maps, we developed a 3D model of the gas distribution. This includes, firstly, a HI component with a low-density superbubble around Cygnus OB2 and, secondly, molecular clouds lying at the edge of the superbubble and in the foreground. We find that a powerful ~50 kyr-old supernova remnant can account for both the morphology and spectrum from 10 TeV-PeV. At PeV energies, the microquasar Cygnus X-3 and diffuse galactic cosmic rays might also contribute to the flux. Below about 10 TeV, hadronic models are incompatible with the expected existence of a superbubble centred on Cygnus OB2. Instead, the spectrum is well fitted with inverse Compton emission from electrons accelerated at stellar-wind termination shocks in Cygnus OB2, which is in line with existing multi-wavelength limits. | ||
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