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
K. P. Arunbabu, St. Albert's College, Ernakulam
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. Brisbois, Michigan Technological UniversityFollow
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
S. Coutiño De León, University of Wisconsin-Madison
C. De León, Universidad Michoacana de San Nicolás de Hidalgo
E. De La Fuente, Universidad de Guadalajara
R. Diaz Hernandez, Instituto Nacional de Astrofisica Optica y Electronica
S. Dichiara, Pennsylvania State University
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
N. Fraija, Universidad Nacional Autónoma de México
A. Galván-Gámez, Universidad Nacional Autónoma de México

Document Type

Article

Publication Date

9-8-2022

Department

Department of Physics

Abstract

Many gamma-ray bursts (GRBs) have been observed from radio wavelengths, and a few at very high energies (VHEs, >100 GeV). The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is well suited to study transient phenomena at VHEs owing to its large field of view and duty cycle. These features allow for searches of VHE emission and can probe different model assumptions of duration and spectra. In this paper, we use data collected by HAWC between 2014 December and 2020 May to search for emission in the energy range from 80 to 800 GeV coming from a sample of 47 short GRBs that triggered the Fermi, Swift, and Konus satellites during this period. This analysis is optimized to search for delayed and extended VHE emission within the first 20 s of each burst. We find no evidence of VHE emission, either simultaneous or delayed, with respect to the prompt emission. Upper limits (90% confidence level) derived on the GRB fluence are used to constrain the synchrotron self-Compton forward-shock model. Constraints for the interstellar density as low as 10-2 cm-3 are obtained when assuming z = 0.3 for bursts with the highest keV fluences such as GRB 170206A and GRB 181222841. Such a low density makes observing VHE emission mainly from the fast-cooling regime challenging.

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/ac880e

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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