Study of the IC 443 region with the HAWC observatory
R. Alfaro, C. Alvarez, M. Araya, J. C. Arteaga-Vel’azquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, A. Bernal, K. S. Caballero-Mora, T. Capistran, A. Carrami~nana, S. Casanova, U. Cotti, J. Cotzomi, S. Couti~no de Le’on, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. D’iaz-V’elez, T. Ergin, C. Espinoza, K. Fang, N. Fraija, S. Fraija, J. A. Garc’ia-Gonz’alez, H. Goksu, J. A. Gonz’alez-Cervera, M. M. Gonz’alez, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hern’andez-Cadena, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. H"untemeyer, S. Kaufmann, A. Lara, J. Lee, H. Le’on Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Mart’inez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostaf’a, M. Najafi, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, M. Osorio, E. Ponce, Y. P’erez Araujo, E. G. P’erez-P’erez, C. D. Rho, D. Rosa-Gonz’alez, M. Roth, E. Ruiz-Velasco, H. Salazar, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, S. Yun-C’arcamo, H. Zhou, C. de Le’on
arXiv:2501.12613v2 Announce Type: replace
Abstract: Supernova remnants are one potential source class considered a PeVatron (i.e. capable of accelerating cosmic rays above PeV energies). The shock fronts produced after the explosion of the supernova are ideal regions for particle acceleration. IC 443 is a supernova remnant that has been studied extensively at different wavelengths. Using 2966 days of gamma-ray data from the HAWC observatory, we study the emission of IC 443 with the objective of finding signatures of cosmic-ray acceleration at the PeV scale. Using a maximum likelihood method, we find a point source located at ($alpha$=94.42$^{circ}$, $delta$=22.35$^{circ}$) that we associate with IC 443. The measured spectrum is a simple power law with an index of $-3.14pm$0.18, which is consistent with previous TeV observations. Although we cannot confirm that IC 443 is a hadronic PeVatron, we do not find any sign that the spectrum has a cut off at tens of TeV energies, with the spectrum extending to $sim$30 TeV. Furthermore, we also find a new extended component in the region whose emission is described by a simple power law with an index of $-2.49pm$0.08 and which we call HAWC J0615+2213. While we show evidence that this new source might be a new TeV halo, we defer a detailed analysis of this new source to another publication.arXiv:2501.12613v2 Announce Type: replace
Abstract: Supernova remnants are one potential source class considered a PeVatron (i.e. capable of accelerating cosmic rays above PeV energies). The shock fronts produced after the explosion of the supernova are ideal regions for particle acceleration. IC 443 is a supernova remnant that has been studied extensively at different wavelengths. Using 2966 days of gamma-ray data from the HAWC observatory, we study the emission of IC 443 with the objective of finding signatures of cosmic-ray acceleration at the PeV scale. Using a maximum likelihood method, we find a point source located at ($alpha$=94.42$^{circ}$, $delta$=22.35$^{circ}$) that we associate with IC 443. The measured spectrum is a simple power law with an index of $-3.14pm$0.18, which is consistent with previous TeV observations. Although we cannot confirm that IC 443 is a hadronic PeVatron, we do not find any sign that the spectrum has a cut off at tens of TeV energies, with the spectrum extending to $sim$30 TeV. Furthermore, we also find a new extended component in the region whose emission is described by a simple power law with an index of $-2.49pm$0.08 and which we call HAWC J0615+2213. While we show evidence that this new source might be a new TeV halo, we defer a detailed analysis of this new source to another publication.