CONSTRAINTS ON THE VERY HIGH ENERGY GAMMA-RAY EMISSION WITH HAWC
- HAWC Collaboration,
- Y. Pérez Araujo(corresponding author)(Author),
- M. M. González(Author),
- N. Fraija(Author),
- A. U. Abeysekara(Author),
- A. Albert(Author)
- Universidad Nacional Autónoma de México,
- University of Utah,
- Los Alamos National Laboratory,
- Universidad Autonoma de Chiapas,
- Universidad Michoacana de San Nicolas de Hidalgo,
- Pennsylvania State University
Research Output:
Chapter in Book/Report/Conference proceeding
Conference contribution
Publication metrics
Metrics
SciVal
Author count
134
SciVal
Paper percentile
20
Abstract
Gamma-ray bursts (GRBs) are among the most luminous sources in the universe. The nature of their emission at TeV energies is one of the most relevant open issues related to these events. The temporal and spectral features inferred from the early and late emissions usually known as prompt and afterglow, respectively, can be interpreted within the context of the fireball model. The synchrotron self-Compton process is expected during the afterglow phase. We explain how the theoretical SSC light curves can be compared with hypothetical upper limit located at z = 0.3. We show the allowed parameter space of the microphysical parameters and density of the circumburst medium. The most restrictive results are obtained when the SSC process lies in the fast cooling regime.
Publication Information
Output type
Research Output:
Chapter in Book/Report/Conference proceeding
Conference contribution
Original language
EnglishPublication milestones
- Published - 18/03/2022
Publication status
Published - 18/03/2022
Volume
395Publication series
- Publisher name: Sissa Medialab Srl
Publication series name: Proceedings of Science
Publication IDs
- Scopus: 85145437869
Host publication title
CONSTRAINTS ON THE VERY HIGH ENERGY GAMMA-RAY EMISSION WITH HAWCAccess to documents
Related Event
Title
37th International Cosmic Ray Conference, ICRC 2021
Event type
ConferenceDate
12/07/2021 - 23/07/2021Location
Virtual, BerlinGermany
Funding Details
de la Universidad Michoacana; Royal Society - Newton Advanced Fellowship 180385; General-itat Valenciana, grant CIDEGENT/2018/034; Chulalongkorn University’s CUniverse (CUAASC) grant; Coordinación General Académica e Innovación (CGAI-UdeG), PRODEP-SEP UDG-CA-499; Institute of Cosmic Ray Research (ICRR), University of Tokyo, H.F. acknowledges support by NASA under award number 80GSFC21M0002. We also acknowledge the significant contributions over many years of Stefan Westerhoff, Gaurang Yodh and Arnulfo Zepeda Dominguez, all deceased members of the HAWC collaboration. Thanks to Scott Delay, Luciano Díaz and Eduardo Murrieta for technical support.
We acknowledge the support from: the US National Science Foundation (NSF); the US Department of Energy Office of High-Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnología (CONACyT), México, grants 271051, 232656, 260378, 179588, 254964, 258865, 243290, 132197, A1-S-46288, A1-S-22784, cátedras 873, 1563, 341, 323, Red HAWC, México; DGAPA-UNAM grants IG101320, IN111716-3, IN111419, IA102019, IN110621, IN110521; VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015; the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Polish Science Centre grant, DEC-2017/27/B/ST9/02272; Coordinación de la Investigación Científica de la Universidad Michoacana; Royal Society - Newton Advanced Fellowship 180385; Generalitat Valenciana, grant CIDEGENT/2018/034; Chulalongkorn University’s CUniverse (CUAASC) grant; Coordinación General Académica e Innovación (CGAI-UdeG), PRODEP-SEP UDG-CA-499; Institute of Cosmic Ray Research (ICRR), University of Tokyo, H.F. acknowledges support by NASA under award number 80GSFC21M0002. We also acknowledge the significant contributions over many years of Stefan Westerhoff, Gaurang Yodh and Arnulfo Zepeda Dominguez, all deceased members of the HAWC collaboration. Thanks to Scott Delay, Luciano Díaz and Eduardo Murrieta for technical support.
We acknowledge the support from: the US National Science Foundation (NSF); the US Department of Energy Office of High-Energy Physics; the Laboratory Directed Research and Development (LDRD) program of Los Alamos National Laboratory; Consejo Nacional de Ciencia y Tecnología (CONACyT), México, grants 271051, 232656, 260378, 179588, 254964, 258865, 243290, 132197, A1-S-46288, A1-S-22784, cátedras 873, 1563, 341, 323, Red HAWC, México; DGAPA-UNAM grants IG101320, IN111716-3, IN111419, IA102019, IN110621, IN110521; VIEP-BUAP; PIFI 2012, 2013, PROFOCIE 2014, 2015; the University of Wisconsin Alumni Research Foundation; the Institute of Geophysics, Planetary Physics, and Signatures at Los Alamos National Laboratory; Polish Science Centre grant, DEC-2017/27/B/ST9/02272; Coordinación de la Investigación Científica
FundersFunding numbers
CUAASC
-Chulalongkorn University's CUniverse
-Coordinación General Académica e Innovación
PRODEP-SEP UDG-CA-499
Coordinación de la Investigación Científica de la Universidad Michoacana
-Institute of Geophysics
-Planetary Physics
-Polish Science Centre
DEC-2017/27/B/ST9/02272
US Department of Energy Office of High-Energy Physics
-Universidad Michoacana
-University of Wisconsin Alumni Research Foundation
-VIEP-BUAP
-NSF
-NASA
80GSFC21M0002
NASA
-LDRD
-LANL
-Royal Society
180385
Royal Society
-CONACYT
271051, A1-S-46288, 254964, 258865, A1-S-22784, 260378, 132197, 179588, 232656, 243290
CONACYT
-GVA
CIDEGENT/2018/034
GVA
-University of Tokyo
-DGAPA, UNAM
IN111419, IG101320, IN111716-3, IN110621, IA102019, IN110521
DGAPA, UNAM
-CIC
-