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Author  |
HAWC Collaboration (Alfaro, R. et al); Coutiño de Leon, S. |
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Title |
HAWC Study on the Ultra-high-energy Gamma-Ray Emissions from the Pulsar Wind Nebula G32.64+0.53 |
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Journal Article |
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Year |
2026 |
Publication |
Astrophysical Journal |
Abbreviated Journal |
Astrophys. J. |
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Volume |
1009 |
Issue |
1 |
Pages |
47 - 11pp |
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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 Ecut >= 2.9 PeV (95% one-sided lower bound). The model also constrains the nebular magnetic field to 4.28 μG, supporting a leptonic PWN origin for the observed UHE emission. |
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Address |
[Alfaro, R.; Belmont-Moreno, E.; Espinoza, C.; Leon Vargas, H.; Perez Araujo, Y.; Pratts, A.; Sandoval, A.; Serna-Franco, J.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City, Mexico, Email: baburish@msu.edu; |
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Publisher |
IOP Publishing Ltd |
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Language |
English |
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Series Volume |
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ISSN |
0004-637x |
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Notes |
WOS:001873966900001 |
Approved |
no |
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Is ISI |
yes |
International Collaboration |
yes |
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Call Number |
IFIC @ pastor @ |
Serial |
7448 |
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