Authors

A. Albert, Los Alamos National Laboratory
R. Alfaro, Universidad Nacional Autónoma de México
C. Alvarez, Universidad Autónoma de Chiapas
J. C. Arteaga-Velázquez, Universidad Michoacana de San Nicolás de Hidalgo
D. Avila Rojas, Universidad Nacional Autónoma de México
H. A.Ayala Solares, Eberly College of Science
R. Babu, Michigan Technological UniversityFollow
E. Belmont-Moreno, Universidad Nacional Autónoma de México
C. Blochwitz, Michigan State University
K. S. Caballero-Mora, Universidad Autónoma de Chiapas
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
O. Chaparro-Amaro, Instituto Politécnico Nacional
U. Cotti, Universidad Michoacana de San Nicolás de Hidalgo
J. Cotzomi, Benemerita Universidad Autonoma de Puebla
E. De la Fuente, Universidad de Guadalajara
C. de León, Universidad Michoacana de San Nicolás de Hidalgo
S. Coutiño de León, University of Wisconsin-Madison
R. Diaz Hernandez, Instituto Nacional de Astrofisica Optica y Electronica
B. L. Dingus, Los Alamos National Laboratory
M. A. DuVernois, University of Wisconsin-Madison
M. Durocher, Los Alamos National Laboratory
J. C. Díaz-Vélez, Universidad de Guadalajara
K. Engel, University of Maryland, College Park
C. Espinoza, Universidad Nacional Autónoma de México
K. L. Fan, University of Maryland, College Park
K. Fang, University of Wisconsin-Madison
N. Fraija, Universidad Nacional Autónoma de México
J. A. García-González, Tecnologico de Monterrey
F. Garfias, Universidad Nacional Autónoma de México

Document Type

Article

Publication Date

11-29-2022

Department

Department of Physics

Abstract

This paper reports on the γ-ray properties of the 2018 Galactic nova V392 Per, spanning photon energies ∼0.1 GeV-100 TeV by combining observations from the Fermi Gamma-ray Space Telescope and the HAWC Observatory. As one of the most rapidly evolving γ-ray signals yet observed for a nova, GeV γ-rays with a power-law spectrum with an index Γ = 2.0 ± 0.1 were detected over 8 days following V392 Per’s optical maximum. HAWC observations constrain the TeV γ-ray signal during this time and also before and after. We observe no statistically significant evidence of TeV γ-ray emission from V392 Per, but present flux limits. Tests disfavor the extension of the Fermi Large Area Telescope spectrum to energies above 5 TeV by 2 standard deviations (95%) or more. We fit V392 Per’s GeV γ-rays with hadronic acceleration models, incorporating optical observations, and compare the calculations with HAWC limits.

Publisher's Statement

© 2022. The Author(s). Published by the American Astronomical Society. Publisher’s version of record: https://doi.org/10.3847/1538-4357/ac966a

Publication Title

Astrophysical Journal

Creative Commons License

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

Version

Publisher's PDF

Included in

Physics Commons

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