ABDOLLAHI, S.; ACERO, F.; ACKERMANN, M.; BALDINI, L.; BALLET, J.; BARBIELLINI, G.; BASTIERI, D.; BELLAZZINI, R.; BERENJI, B.; BERRETTA, A.; BISSALDI, E.; BLANDFORD, R.D.; BONINO, R.; BRUEL, P.; BUSON, S.; CAMERON, R.A.; CAPUTO, R.; CARAVEO, P.A.; CASTRO, D.; CHIARO, G.; CIBRARIO, N.; CIPRINI, S.; CORONADO-BLÁZQUEZ, J.; CRNOGORCEVIC, M.; CUTINI, S.; D'AMMANDO, F.; DE GAETANO, S.; DI LALLA, N.; DIRIRSA, F.; DI VENERE, L.; DOMÍNGUEZ, A.; FEGAN, S.J.; FIORI, A.; FLEISCHHACK, H.; FRANCKOWIAK, A.; FUKAZAWA, Y.; FUSCO, P.; GAMMALDI, V.; GARGANO, F.; GASPARRINI, D.; GIACCHINO, F.; GIGLIETTO, N.; GIORDANO, F.; GIROLETTI, M.; GLANZMAN, T.; GREEN, D.; GRENIER, I.A.; GRONDIN, M.-H.; GUIRIEC, S.; GUSTAFSSON, M.; HARDING, A.K.; HAYS, E.; HEWITT, J.W.; HORAN, D.; HOU, X.; JÓHANNESSON, G.; KAYANOKI, T.; KERR, M.; KUSS, M.; LARSSON, S.; LATRONICO, L.; LEMOINE-GOUMARD, M.; LI, J.; LONGO, F.; LOPARCO, F.; LUBRANO, P.; MALDERA, S.; MALYSHEV, D.; MANFREDA, A.; MARTÍ-DEVESA, G.; MAZZIOTTA, M.N.; MEREU, I.; MICHELSON, P.F.; MIRABAL, N.; MITTHUMSIRI, W.; MIZUNO, T.; MONZANI, M.E.; MORSELLI, A.; MOSKALENKO, I.V.; NUSS, E.; OMODEI, N.; ORIENTI, M.; ORLANDO, E.; ORMES, J.F.; PANEQUE, D.; PEI, Z.; PERSIC, M.; PESCE-ROLLINS, M.; PILLERA, R.; POON, H.; PORTER, T.A.; PRINCIPE, G.; RAINÒ, S.; RANDO, R.; RANI, B.; RAZZANO, M.; RAZZAQUE, S.; REIMER, A.; REIMER, O.; REPOSEUR, T.; SÁNCHEZ-CONDE, M.; PARKINSON SAZ, P.M.; SCOTTON, L.; SERINI, D.; SGRÒ, C.; SISKIND, E.J.; SPANDRE, G.; SPINELLI, P.; SUEOKA, K.; SUSON, D.J.; TAJIMA, H.; TAK, D.; THAYER, J.B.; TORRES, D.F.; TROJA, E.; VALVERDE, J.; WADIASINGH, Z.; WOOD, K.; ZAHARIJAS, G.

doi:10.3847/1538-4357/ac704f

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ABDOLLAHI, S.
Institut de recherche en astrophysique et planétologie [IRAP]

ACERO, F.
Astrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]

ACKERMANN, M.

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Astrophys.J. 2022, vol. 933, n° 2, p. 204

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Cosmic rays are mostly composed of protons accelerated to relativistic speeds. When those protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma-rays. This offers a compelling way to identify the acceleration sites of protons. A characteristic hadronic spectrum, with a low-energy break around 200 MeV, was detected in the gamma-ray spectra of four supernova remnants (SNRs), IC 443, W44, W49B, and W51C, with the Fermi Large Area Telescope. This detection provided direct evidence that cosmic-ray protons are (re-)accelerated in SNRs. Here, we present a comprehensive search for low-energy spectral breaks among 311 4FGL catalog sources located within 5° from the Galactic plane. Using 8 yr of data from the Fermi Large Area Telescope between 50 MeV and 1 GeV, we find and present the spectral characteristics of 56 sources with a spectral break confirmed by a thorough study of systematic uncertainty. Our population of sources includes 13 SNRs for which the proton–proton interaction is enhanced by the dense target material; the high-mass gamma-ray binary LS I+61 303; the colliding wind binary η Carinae; and the Cygnus star-forming region. This analysis better constrains the origin of the gamma-ray emission and enlarges our view to potential new cosmic-ray acceleration sites.< Réduire

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Search for New Cosmic-Ray Acceleration Sites within the 4FGL Catalog Galactic Plane Sources

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