HAWC Study on the Ultra-high-energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53

Abstract 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 nonthermal 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 multiwavelength 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 cut ≥ 2.9 PeV (95% one-sided lower bound). The model also constrains the nebular magnetic field to 4.28 μ G, supporting a leptonic PWN origin for the observed UHE emission.

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Journal
The Astrophysical Journal
Published
2026-09-14
DOI
https://doi.org/10.3847/1538-4357/ae975c
Primary Topic
Astrophysics and Cosmic Phenomena
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article
Field-Weighted Citation Impact
0.00

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article

HAWC Study on the Ultra-high-energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53

H. Zhou, J. A. Morales-Soto, Daniel Salazar-Gallegos, Enrique Varela et al.
The Astrophysical Journal
Astrophysics and Cosmic Phenomena
article

HAWC Study on the Ultra-high-energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53

H. Zhou, J. A. Morales-Soto, Daniel Salazar-Gallegos, Enrique Varela, E. Moreno, R. Torres-Escobedo, P. Miranda-Romagnoli, K. Malone, L. Nellen, Sarah Recchia, O. Tibolla, J. Martínez-Castro, I. Torres, G. Luis-Raya, Kirsten Tollefson, E. G. Pérez‐Pérez, H. León Vargas, A. Sandoval, A. J. Smith, R. W. Springer, R. Noriega-Papaqui, Chang Dong Rho, D. Rosa‐González, A. L. Longinotti, Alvaro Pratts, M. Mostafá, L. Villaseñor, John A. Matthews, X. Wang, M. Schneider, I. J. Watson, Humberto Antonio Salazar Ibarguen, N. Omodei, F. Carreón, S. Coutiño de León, F. Hueyotl-Zahuantitla, R. Babu, J. C. Arteaga-Velázquez, U. Cotti, M. A. DuVernois, R. Diaz Hernandez, P. Bangale, C. Alvarez, F. Garfias, S. Fraija, E. Anita-Rangel, T. Ergin, J. P. Harding, J. Cotzomi, E. Belmont-Moreno, J. A. García-González, D. Guevel, D. Huang, C. Espinoza, H. A. Ayala Solares, M. Araya, J. C. Díaz-Vélez, I. Herzog, J. Becerra González, T. Capistrán, N. Fraija, A. Carramiñana, E. De la Fuente, J. Gyeong, D. Avila Rojas, J. A. Goodman, P. Desiati, M. Molero Gonzalez, N. Ghosh, S. Casanova, R. Alfaro, K. S. Caballero-Mora, J. Lee, N. Di Lalla, K. Engel, A. Bernal, E. G. Pérez-Pérez, J. Lee, K. Tollefson, A. Iriarte, K. Leavitt, D. Kieda, J. Martínez-Castro, H. León Vargas, P. Hüntemeyer, S. Kaufmann, E. Ponce, J. Serna-Franco, S. Yu, A. Rodriguez Parra, M. Najafi, M. Shin, X. Zhang, Z. Wang, A. Nayerhoda, M. Roth
article en

Abstract

Abstract 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 nonthermal 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 multiwavelength 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 cut ≥ 2.9 PeV (95% one-sided lower bound). The model also constrains the nebular magnetic field to 4.28 μ G, supporting a leptonic PWN origin for the observed UHE emission.

The Astrophysical JournalVol. 1009(1)
Universidad Autónoma del Estado de Hidalgo (MX), Michigan Technological University (US), University of Seoul (KR), Pennsylvania State University (US), Los Alamos National Laboratory (US), Universitat de València (ES), Universidad Michoacana de San Nicolás de Hidalgo (MX), Shanghai Jiao Tong University (CN), Missouri University of Science and Technology (US), University of Utah (US), Temple College (US), Universidad de Costa Rica (CR), Universidad Politécnica de Pachuca (MX), Institute of Nuclear Physics, Polish Academy of Sciences (PL), Exact Sciences (United States) (US), Universidad Autónoma de Chiapas (MX), Laboratório Nacional de Astrofísica (BR), University of Turin (IT), Instituto Politécnico Nacional (MX), University of Maryland, College Park (US), Benemérita Universidad Autónoma de Puebla (MX), Temple University (US), Sungkyunkwan University (KR), University of Delaware (US), Michigan State University (US), Universidad Nacional Autónoma de México (MX), Stanford University (US), Tecnológico de Monterrey (MX)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, European Commission, National Research Foundation, Consejo Nacional de Ciencia y Tecnología, National Research Foundation of Korea, Benemérita Universidad Autónoma de Puebla, Office of National Higher Education Science Research and Innovation Policy Council, Dirección General de Asuntos del Personal Académico, Universidad Nacional Autónoma de México, Coordinación de la Investigación Científica, Institute for Cosmic Ray Research, University of Tokyo, Laboratory Directed Research and Development, Los Alamos National Laboratory
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