Home > Publications database > Study of the GeV to TeV morphology of the γ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT - Evidence for cosmic ray escape > print

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024 7 _ |a 10.1051/0004-6361/202038748
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024 7 _ |a MAGIC:2020bim
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024 7 _ |a inspire:1827379
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024 7 _ |a 0004-6361
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024 7 _ |a 1432-0746
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024 7 _ |a arXiv:2010.15854
|2 arXiv
024 7 _ |a 10.3204/PUBDB-2023-01336
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037 _ _ |a PUBDB-2023-01336
041 _ _ |a English
082 _ _ |a 520
088 _ _ |a arXiv:2010.15854
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100 1 _ |a Acciari, V. A.
|b 0
245 _ _ |a Study of the GeV to TeV morphology of the γ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT - Evidence for cosmic ray escape
260 _ _ |a Les Ulis
|c 2023
|b EDP Sciences
336 7 _ |a article
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336 7 _ |a Output Types/Journal article
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336 7 _ |a Journal Article
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336 7 _ |a ARTICLE
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336 7 _ |a Journal Article
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500 _ _ |a A&A 670, A8 (2023). 20 pages, 10 figures. Accepted for publication in A&A. Corresponding authors: M. Strzys, G. Morlino, S. Masuda, and I. Vovk
520 _ _ |a Context. Diffusive shock acceleration (DSA) is the most promising mechanism that accelerates Galactic cosmic rays (CRs) in the shocks of supernova remnants (SNRs). It is based on particles scattering caused by turbulence ahead and behind the shock. The turbulence upstream is supposedly generated by the CRs, but this process is not well understood. The dominant mechanism may depend on the evolutionary state of the shock and can be studied via the CRs escaping upstream into the interstellar medium (ISM).Aims. Previous observations of the γ Cygni SNR showed a difference in morphology between GeV and TeV energies. Since this SNR has the right age and is at the evolutionary stage for a significant fraction of CRs to escape, our aim is to understand γ-ray emission in the vicinity of the γ Cygni SNR.Methods. We observed the region of the γ Cygni SNR with the MAGIC Imaging Atmospheric Cherenkov telescopes between 2015 May and 2017 September recording 87 h of good-quality data. Additionally, we analysed Fermi-LAT data to study the energy dependence of the morphology as well as the energy spectrum in the GeV to TeV range. The energy spectra and morphology were compared against theoretical predictions, which include a detailed derivation of the CR escape process and their γ-ray generation.Results. The MAGIC and Fermi-LAT data allowed us to identify three emission regions that can be associated with the SNR and that dominate at different energies. Our hadronic emission model accounts well for the morphology and energy spectrum of all source components. It constrains the time-dependence of the maximum energy of the CRs at the shock, the time-dependence of the level of turbulence, and the diffusion coefficient immediately outside the SNR shock. While in agreement with the standard picture of DSA, the time-dependence of the maximum energy was found to be steeper than predicted, and the level of turbulence was found to change over the lifetime of the SNR.Key words: acceleration of particles / cosmic rays / gamma rays: general / gamma rays: ISM / ISM: clouds / ISM: supernova remnants★ Corresponding authors; e-mail: contact.magic@mpp.mpg.de
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650 _ 7 |a emission: model
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650 _ 7 |a cosmic radiation: galaxy
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650 _ 7 |a acceleration: shock waves
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650 _ 7 |a time dependence
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650 _ 7 |a energy spectrum
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650 _ 7 |a turbulence
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650 _ 7 |a gamma ray
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650 _ 7 |a MAGIC
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650 _ 7 |a GLAST
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650 _ 7 |a GeV
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650 _ 7 |a TeV
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650 _ 7 |a inverse scattering method
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650 _ 7 |a energy dependence
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650 _ 7 |a Cherenkov counter
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650 _ 7 |a diffusion
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650 _ 7 |a supernova
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650 _ 7 |a lifetime
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650 _ 7 |a imaging
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773 _ _ |a 10.1051/0004-6361/202038748
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787 0 _ |a Acciari, V. A. et.al.
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|t Study of the GeV to TeV morphology of the $\gamma$ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT - Evidence for cosmic ray escape
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