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Main Authors: Alfaro, R., Alvarez, C., Anita-Rangel, E., Araya, M., Arteaga-Velázquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Babu, R., Bangale, P., Belmont-Moreno, E., Bernal, A., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Carreón, F., Casanova, S., Cotti, U., Cotzomi, J., de León, S. Coutiño, De la Fuente, E., Desiati, P., Di Lalla, N., Hernandez, R. Diaz, DuVernois, M. A., Díaz-Vélez, J. C., Engel, K., Ergin, T., Espinoza, C., Fraija, N., Fraija, S., García-González, J. A., Garfias, F., Ghosh, N., González, M. M., González, J. A., Goodman, J. A., Guevel, D., Gyeong, J., Harding, J. P., Herzog, I., Huang, D., Hueyotl-Zahuantitla, F., Iriarte, A., Kaufmann, S., Kieda, D., Leavitt, K., Lee, W. H., Lee, J., Vargas, H. León, Longinotti, A. L., Luis-Raya, G., Malone, K., Martinez, O., Martínez-Castro, J., Matthews, J. A., Miranda-Romagnoli, P., Morales-Soto, J. A., Moreno, E., Mostafá, M., Najafi, M., Nayerhoda, A., Nellen, L., Noriega-Papaqui, R., Omodei, N., Ponce, E., Araujo, Y. Pérez, Pérez-Pérez, E. G., Rho, C. D., Parra, A. Rodriguez, Rosa-González, D., Roth, M., Salazar, H., Salazar-Gallegos, D., Sandoval, A., Schneider, M., Serna-Franco, J., Shin, M., Smith, A. J., Son, Y., Springer, R. W., Tibolla, O., Tollefson, K., Torres, I., Torres-Escobedo, R., Varela, E., Villaseñor, L., Wang, X., Wang, Z., Watson, I. J., Yu, S., Zhang, X., Zhou, H., de León, C.
Format: Preprint
Published: 2026
Subjects:
High Energy Astrophysical Phenomena
Online Access:https://arxiv.org/abs/2603.19721
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Table of Contents:
  • Multi-TeV gamma-ray emission around eHWC J1850+001 (a source from the first HAWC catalog of gamma-ray sources emitting above 56 TeV) is spatially coincident with the pulsar wind nebula (PWN) G32.64+0.53, powered by PSR J1849-0001. The absence of counterparts in radio, optical, and GeV energy ranges, contrasted with clear detections in X-rays and very-high-energy (VHE) gamma-rays, is indicative of a non-thermal leptonic origin for the nebula. We apply a systematic analysis pipeline, including a sophisticated model for the Galactic diffuse emission, to 2860 days of data from the HAWC Observatory. Our detailed analysis confirms that the ultra-high-energy (UHE) emission originates from G32.64+0.53, and we measure its spectrum up to 270 TeV with significant emission well beyond 100 TeV. We fit the multi-wavelength observations with a time-dependent leptonic model powered by the pulsar's rotational energy, and the results establish the nebula as a leptonic PeV accelerator, capable of accelerating electrons to a maximum energy of $E_{\mathrm{cut}}=1.5_{-0.6}^{+1.7}~\mathrm{PeV}$. The model also constrains the true age of the system to $26.8~\mathrm{kyr}$ and the nebular magnetic field to a low value of $2.5 ~\mathrm{μG}$, supporting a leptonic PWN origin for the observed UHE emission.

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