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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.
פורמט:	Preprint
יצא לאור:	2026
נושאים:	High Energy Astrophysical Phenomena
גישה מקוונת:	https://arxiv.org/abs/2603.19721
תגים:	הוספת תג אין תגיות, היה/י הראשונ/ה לתייג את הרשומה!

_version_	1866915877405851648
author	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.
author_facet	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.
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.
format	Preprint
id	arxiv_https___arxiv_org_abs_2603_19721
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	HAWC Study on the Ultra-High-Energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53 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. High Energy Astrophysical Phenomena 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.
title	HAWC Study on the Ultra-High-Energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53
topic	High Energy Astrophysical Phenomena
url	https://arxiv.org/abs/2603.19721

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