期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 896, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/2041-8213/ab96cc
关键词
Gamma-ray astronomy; Gamma-ray sources; Gamma-rays; Cosmic ray sources; Supernova remnants; Gamma-ray observatories
资金
- US National Science Foundation (NSF)
- US Department of Energy Office of High-Energy Physics
- Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory
- Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico [271051, 232656, 260378, 179588, 254964, 258865, 243290, 132197, A1-S-46288, A1-S-22784, 873, 1563, 323, 341]
- DGAPA-UNAM [IG101320, IN111315, IN111716-3, IN111419, IA102019, IN112218]
- VIEP-BUAP
- PIFI 2012, 2013
- PROFOCIE 2014, 2015
- University of Wisconsin Alumni Research Foundation
- Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory
- Polish Science Centre [DEC-2017/27/B/ST9/02272]
- Coordinacion de la Investigacion Cientifica de la Universidad Michoacana
- Royal Society-Newton Advanced Fellowship [180385]
- Generalitat Valenciana, Spain [CIDEGENT/2018/034]
We present the detection of very-high-energy gamma-ray emission above 100 TeV from HAWC J2227+610 with the High-Altitude Water Cherenov Gamma-Ray Observatory (HAWC) observatory. Combining our observations with previously published results by the Very Energetic Radiation Imaging Telescope Array System (VERTIAS), we interpret the gamma-ray emission from HAWC J2227+610 as emission from protons with a lower limit in their cutoff energy of 800 TeV. The most likely source of the protons is the associated supernova remnant G106.3+2.7, making it a good candidate for a Galactic PeVatron. However, a purely leptonic origin of the observed emission cannot be excluded at this time.
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