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000580601 0247_ $$2doi$$a10.1051/0004-6361/202038748
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000580601 0247_ $$2arXiv$$aarXiv:2010.15854
000580601 0247_ $$2datacite_doi$$a10.3204/PUBDB-2023-01336
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000580601 041__ $$aEnglish
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000580601 088__ $$2arXiv$$aarXiv:2010.15854
000580601 1001_ $$aAcciari, V. A.$$b0
000580601 245__ $$aStudy 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
000580601 260__ $$aLes Ulis$$bEDP Sciences$$c2023
000580601 3367_ $$2DRIVER$$aarticle
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000580601 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1679920033_2396
000580601 3367_ $$2BibTeX$$aARTICLE
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000580601 3367_ $$00$$2EndNote$$aJournal Article
000580601 500__ $$aA&A 670, A8 (2023). 20 pages, 10 figures. Accepted for publication in A&A. Corresponding authors: M. Strzys, G. Morlino, S. Masuda, and I. Vovk
000580601 520__ $$aContext. 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
000580601 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
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000580601 650_7 $$2INSPIRE$$aemission: model
000580601 650_7 $$2INSPIRE$$acosmic radiation: galaxy
000580601 650_7 $$2INSPIRE$$aacceleration: shock waves
000580601 650_7 $$2INSPIRE$$atime dependence
000580601 650_7 $$2INSPIRE$$aenergy spectrum
000580601 650_7 $$2INSPIRE$$aturbulence
000580601 650_7 $$2INSPIRE$$agamma ray
000580601 650_7 $$2INSPIRE$$aMAGIC
000580601 650_7 $$2INSPIRE$$aGLAST
000580601 650_7 $$2INSPIRE$$aGeV
000580601 650_7 $$2INSPIRE$$aTeV
000580601 650_7 $$2INSPIRE$$ainverse scattering method
000580601 650_7 $$2INSPIRE$$aenergy dependence
000580601 650_7 $$2INSPIRE$$aCherenkov counter
000580601 650_7 $$2INSPIRE$$adiffusion
000580601 650_7 $$2INSPIRE$$asupernova
000580601 650_7 $$2INSPIRE$$alifetime
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000580601 693__ $$0EXP:(DE-H253)MAGIC-20170101$$5EXP:(DE-H253)MAGIC-20170101$$eMajor Atmospheric Gamma Imaging Cherenkov$$x0
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000580601 7001_ $$aAntonelli, L. A.$$b2
000580601 7001_ $$aArbet Engels, A.$$b3
000580601 7001_ $$aBaack, D.$$b4
000580601 7001_ $$aBabić, A.$$b5
000580601 7001_ $$aBanerjee, B.$$b6
000580601 7001_ $$0INSPIRE-00571806$$aBarres de Almeida, U.$$b7
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000580601 7001_ $$aCelli, S.$$b182
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000580601 7870_ $$0PUBDB-2023-01414$$aAcciari, V. A. et.al.$$d2023$$iIsParent$$rarXiv:2010.15854$$tStudy 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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