HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet Pulsar

Authors

• A. Albert, Los Alamos National Laboratory
• R. Alfaro, Universidad Nacional Autónoma de México
• J. C. Arteaga-Velázquez, Universidad Michoacana de San Nicolás de Hidalgo
• H. A. Ayala Solares, Eberly College of Science
• E. Belmont-Moreno, Universidad Nacional Autónoma de México
• T. Capistrán, Universidad Nacional Autónoma de México
• A. Carramiñana, Instituto Nacional de Astrofisica Optica y Electronica
• S. Casanova, Henryk Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences
• J. Cotzomi, Benemerita Universidad Autonoma de Puebla
• S. Coutiño De León, University of Wisconsin-Madison
• E. De la Fuente, Universidad de Guadalajara
• C. de León, Universidad Michoacana de San Nicolás de Hidalgo
• R. Diaz Hernandez, Instituto Nacional de Astrofisica Optica y Electronica
• M. A. DuVernois, University of Wisconsin-Madison
• J. C. Díaz-Vélez, Universidad de Guadalajara
• C. Espinoza, Universidad Nacional Autónoma de México
• K. L. Fan, University of Maryland, College Park
• N. Fraija, Universidad Nacional Autónoma de México
• K. Fang, University of Wisconsin-Madison
• J. A. García-González, Tecnologico de Monterrey
• F. Garfias, Universidad Nacional Autónoma de México
• A. Jardin-Blicq, LP2I - Laboratoire de Physique des Deux Infinis Bordeaux
• M. M. González, Universidad Nacional Autónoma de México
• J. A. Goodman, University of Maryland, College Park
• J. P. Harding, Los Alamos National Laboratory
• S. Hernandez, Universidad Nacional Autónoma de México
• D. Huang, Michigan Technological UniversityFollow
• F. Hueyotl-Zahuantitla, Universidad Autónoma de Chiapas
• P. Hüntemeyer, Michigan Technological UniversityFollow
• A. Iriarte, Universidad Nacional Autónoma de México
• V. Joshi, Friedrich-Alexander-Universität Erlangen-Nürnberg
• et. al.

Document Type

Article

Publication Date

2-15-2023

Department

Department of Physics

Abstract

Extended very-high-energy (VHE; 0.1-100 TeV) γ-ray emission has been observed around several middle-aged pulsars and referred to as “TeV halos.” Their formation mechanism remains under debate. It is also unknown whether they are ubiquitous or related to a certain subgroup of pulsars. With 2321 days of observation, the High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory detected VHE γ-ray emission at the location of the radio-quiet pulsar PSR J0359+5414 with >6σ significance. By performing likelihood tests with different spectral and spatial models and comparing the TeV spectrum with multiwavelength observations of nearby sources, we show that this excess is consistent with a TeV halo associated with PSR J0359+5414, though future observation of HAWC and multiwavelength follow-ups are needed to confirm this nature. This new halo candidate is located in a noncrowded region in the outer galaxy. It shares similar properties to the other halos but its pulsar is younger and radio-quiet. Our observation implies that TeV halos could commonly exist around pulsars and their formation does not depend on the configuration of the pulsar magnetosphere.

Publisher's Statement

© 2023. The Author(s). Published by the American Astronomical Society. Publisher’s version of record: https://doi.org/10.3847/2041-8213/acb5ee

Publication Title

Astrophysical Journal Letters

Recommended Citation

Albert, A., Alfaro, R., Arteaga-Velázquez, J., Ayala Solares, H., Belmont-Moreno, E., Capistrán, T., Carramiñana, A., Casanova, S., Cotzomi, J., De León, S., Fuente, E., de León, C., Diaz Hernandez, R., DuVernois, M., Díaz-Vélez, J., Espinoza, C., Fan, K., Fraija, N., Fang, K., García-González, J., Garfias, F., Jardin-Blicq, A., González, M., Goodman, J., Harding, J., Hernandez, S., Huang, D., Hueyotl-Zahuantitla, F., Hüntemeyer, P., Iriarte, A., Joshi, V., & et. al. (2023). HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet Pulsar. Astrophysical Journal Letters, 944(2). http://doi.org/10.3847/2041-8213/acb5ee
Retrieved from: https://digitalcommons.mtu.edu/michigantech-p/16889

Creative Commons License

This work is licensed under a Creative Commons Attribution 4.0 International License.

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