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Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415

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Depaoli,  D.       
Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society;

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Ruiz-Velasco,  E.       
Division Prof. Dr. James A. Hinton, MPI for Nuclear Physics, Max Planck Society;

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Citation

HAWC Collaboration, Alfaro, R., Alvarez, C., Arteaga-Velázquez, J. C., Avila Rojas, D., Ayala Solares, H. A., et al. (2024). Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415. The Astrophysical Journal, 975: 198. doi:10.3847/1538-4357/ad782a.


Cite as: https://hdl.handle.net/21.11116/0000-0010-43E5-0
Abstract
The first TeV γ-ray source with no lower energy counterparts, TeV J2032+4130, was discovered by HEGRA. It appears in the third HAWC catalog as 3HWC J2031+415 and it is a bright TeV γ-ray source whose emission has previously been resolved as two sources: HAWC J2031+415 and HAWC J2030+409. While HAWC J2030+409 has since been associated with the Fermi Large Area Telescope Cygnus Cocoon, no such association for HAWC J2031+415 has yet been found. In this work, we investigate the spectrum and energy-dependent morphology of HAWC J2031+415. We associate HAWC J2031+415 with a γ-ray binary system containing the pulsar PSR J2032+4127 and its companion MT91 213. We study HAWC data to observe their periastron in 2017. Additionally, we perform a combined multiwavelength analysis using radio, X-ray, and γ-ray emission. We conclude that HAWC J2031+415 and, by extension, TeV J2032+4130 are most probably a pulsar wind nebula powered by PSR J2032+4127.