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We acknowledge support from the US National Science Foundation (NSF); the US Department of Energy Office of High-Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnologia (CONACyT), Mexico, grants 271051, 232656, 260378, 179588, 254964, 258865, 243290, 132197, A1-S-46288, A1-S-22784, catedras 873, 1563, 341, 323, Red HAWC, Mexico; DGAPA-UNAM grants IG101320, IN111315, IN111716-3, IN111419, IA102019, IN112218; VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015; the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Polish Science Centre grant, DEC-2017/27/B/ST9/02272; Coordinacion de la Investigacion Cientifica de la Universidad Michoacana; Royal Society-Newton Advanced Fellowship 180385; Generalitat Valenciana, grant CIDEGENT/2018/034; Chulalongkorn University's CUniverse (CUAASC) grant. Thanks to Scott Delay, Luciano Diaz, and Eduardo Murrieta for technical support.

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Evidence of 200 TeV Photons from HAWC J1825-134

Publicado en:Astrophysical Journal Letters. 907 (2): L30- - 2021-02-01 907(2), DOI: 10.3847/2041-8213/abd77b

Autores: Albert, A.; Alfaro, R.; Alvarez, C.; Camacho, J. R. Angeles; Arteaga-Velazquez, J. C.; Arunbabu, K. P.; Rojas, D. Avila; Ayala Solares, H. A.; Baghmanyan, V.; Belmont-Moreno, E.; BenZvi, S. Y.; Brisbois, C.; Capistran, T.; Carraminana, A.; Casanova, S.; Cotti, U.; Cotzomi, J.; Fuente, E. De la; Hernandez, R. Diaz; Dingus, B. L.; DuVernois, M. A.; Durocher, M.; Diaz-Velez, J. C.; Engel, K.; Espinoza, C.; Fang, K.; Fleischhack, H.; Fraija, N.; Galvan-Gamez, A.; Garcia, D.; Garcia-Gonzalez, J. A.; Garfias, F.; Giacinti, G.; Gonzalez, M. M.; Goodman, J. A.; Harding, J. P.; Hona, B.; Huang, D.; Hueyotl-Zahuantitla, F.; Huntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Kunde, G. J.; Lara, A.; Lee, W. H.; Vargas, H. Leon; Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; Lundeen, J.; Malone, K.; Marandon, V.; Martinez, O.; Martinez-Castro, J.; Matthews, J. A.; Miranda-Romagnoli, P.; Moreno, E.; Mostafa, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Omodei, N.; Peisker, A.; Araujo, Y. Perez; Perez-Perez, E. G.; Rho, C. D.; Rosa-Gonzalez, D.; Salazar, H.; Greus, F. Salesa; Sandoval, A.; Schneider, M.; Serna, F.; Springer, R. W.; Tollefson, K.; Torres, I.; Torres-Escobedo, R.; Urena-Mena, F.; Villasenor, L.; Willox, E.; Zhou, H.; de Leon, C.;

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Resumen

The Earth is bombarded by ultrarelativistic particles, known as cosmic rays (CRs). CRs with energies up to a few PeV (=10(15) eV), the knee in the particle spectrum, are believed to have a Galactic origin. One or more factories of PeV CRs, or PeVatrons, must thus be active within our Galaxy. The direct detection of PeV protons from their sources is not possible since they are deflected in the Galactic magnetic fields. Hundred TeV gamma-rays from decaying pi(0), produced when PeV CRs collide with the ambient gas, can provide the decisive evidence of proton acceleration up to the knee. Here we report the discovery by the High Altitude Water Cerenkov (HAWC) observatory of the gamma-ray source, HAWC J1825-134, whose energy spectrum extends well beyond 200 TeV without a break or cutoff. The source is found to be coincident with a giant molecular cloud. The ambient gas density is as high as 700 protons cm(-3). While the nature of this extreme accelerator remains unclear, CRs accelerated to energies of several PeV colliding with the ambient gas likely produce the observed radiation.

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