H.E.S.S. follow-up observations of GRB 221009A

F. Aharonian; F. A. Benkhali; J. Aschersleben; H. Ashkar; M. Backes; A. Baktash; V. B. Martins; R. Batzofin; Y. Becherini; D. Berge; K. Bernlöhr; B. Bi; M. Böttcher; C. Boisson; J. Bolmont; M. de Bony de Lavergne; J. Borowska; M. Bouyahiaoui; F. Bradascio; M. Breuhaus; R. Brose; F. Brun; B. Bruno; T. Bulik; C. Burger-Scheidlin; S. Caroff; S. Casanova; J. Celic; M. Cerruti; T. Chand; S. Chandra; A. Chen; J. Chibueze; O. Chibueze; G. Cotter; S. Dai; J. D. Mbarubucyeye; J. Devin; A. Djannati-Ataï; A. Dmytriiev; V. Doroshenko; K. Egberts; S. Einecke; J.-P. Ernenwein; S. Fegan; G. Fichet de Clairfontaine; M. Filipovic; G. Fontaine; M. Füßling; S. Funk; null et al

H.E.S.S. follow-up observations of GRB 221009A

F. Aharonian, F. A. Benkhali, J. Aschersleben, H. Ashkar, M. Backes, A. Baktash, V. B. Martins, R. Batzofin, Y. Becherini, D. Berge, K. Bernlöhr, B. Bi, M. Böttcher, C. Boisson, J. Bolmont, M. de Bony de Lavergne, J. Borowska, M. Bouyahiaoui, F. Bradascio, M. BreuhausR. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, S. Dai, J. D. Mbarubucyeye, J. Devin, A. Djannati-Ataï, A. Dmytriiev, V. Doroshenko, K. Egberts, S. Einecke, J.-P. Ernenwein, S. Fegan, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füßling, S. Funk, et al

Western Sydney University

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Abstract

GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE; >100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of Î¦ UL 95 % = 9.7 Ã— 10 âˆ’ 12 erg cm âˆ’ 2 s âˆ’ 1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.

Original language	English
Article number	L27
Number of pages	8
Journal	Astrophysical Journal Letters
Volume	946
Issue number	1
Publication status	Published - 1 Mar 2023

Bibliographical note

Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.

Open Access - Access Right Statement

Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence (https://creativecommons.org/licenses/by/4.0/). Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

Cite this

Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Baktash, A., Martins, V. B., Batzofin, R., Becherini, Y., Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., de Bony de Lavergne, M., Borowska, J., Bouyahiaoui, M., Bradascio, F., ... et al (2023). H.E.S.S. follow-up observations of GRB 221009A. Astrophysical Journal Letters, 946(1), Article L27.

@article{a54028054365462dabde5df657fb2587,

title = "H.E.S.S. follow-up observations of GRB 221009A",

abstract = "GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE; >100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of {\^I}¦ UL 95 % = 9.7 {\~A}— 10 {\^a}ˆ{\textquoteright} 12 erg cm {\^a}ˆ{\textquoteright} 2 s {\^a}ˆ{\textquoteright} 1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.",

author = "F. Aharonian and Benkhali, {F. A.} and J. Aschersleben and H. Ashkar and M. Backes and A. Baktash and Martins, {V. B.} and R. Batzofin and Y. Becherini and D. Berge and K. Bernl{\"o}hr and B. Bi and M. B{\"o}ttcher and C. Boisson and J. Bolmont and {de Bony de Lavergne}, M. and J. Borowska and M. Bouyahiaoui and F. Bradascio and M. Breuhaus and R. Brose and F. Brun and B. Bruno and T. Bulik and C. Burger-Scheidlin and S. Caroff and S. Casanova and J. Celic and M. Cerruti and T. Chand and S. Chandra and A. Chen and J. Chibueze and O. Chibueze and G. Cotter and S. Dai and Mbarubucyeye, {J. D.} and J. Devin and A. Djannati-Ata{\"i} and A. Dmytriiev and V. Doroshenko and K. Egberts and S. Einecke and J.-P. Ernenwein and S. Fegan and {Fichet de Clairfontaine}, G. and M. Filipovic and G. Fontaine and M. F{\"u}{\ss}ling and S. Funk and {et al}",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = mar,

day = "1",

language = "English",

volume = "946",

journal = "Astrophysical Journal Letters",

issn = "2041-8205",

publisher = "Institute of Physics Publishing",

number = "1",

}

Aharonian, F, Benkhali, FA, Aschersleben, J, Ashkar, H, Backes, M, Baktash, A, Martins, VB, Batzofin, R, Becherini, Y, Berge, D, Bernlöhr, K, Bi, B, Böttcher, M, Boisson, C, Bolmont, J, de Bony de Lavergne, M, Borowska, J, Bouyahiaoui, M, Bradascio, F, Breuhaus, M, Brose, R, Brun, F, Bruno, B, Bulik, T, Burger-Scheidlin, C, Caroff, S, Casanova, S, Celic, J, Cerruti, M, Chand, T, Chandra, S, Chen, A, Chibueze, J, Chibueze, O, Cotter, G, Dai, S, Mbarubucyeye, JD, Devin, J, Djannati-Ataï, A, Dmytriiev, A, Doroshenko, V, Egberts, K, Einecke, S, Ernenwein, J-P, Fegan, S, Fichet de Clairfontaine, G, Filipovic, M, Fontaine, G, Füßling, M, Funk, S & et al 2023, 'H.E.S.S. follow-up observations of GRB 221009A', Astrophysical Journal Letters, vol. 946, no. 1, L27.

TY - JOUR

T1 - H.E.S.S. follow-up observations of GRB 221009A

AU - Aharonian, F.

AU - Benkhali, F. A.

AU - Aschersleben, J.

AU - Ashkar, H.

AU - Backes, M.

AU - Baktash, A.

AU - Martins, V. B.

AU - Batzofin, R.

AU - Becherini, Y.

AU - Berge, D.

AU - Bernlöhr, K.

AU - Bi, B.

AU - Böttcher, M.

AU - Boisson, C.

AU - Bolmont, J.

AU - de Bony de Lavergne, M.

AU - Borowska, J.

AU - Bouyahiaoui, M.

AU - Bradascio, F.

AU - Breuhaus, M.

AU - Brose, R.

AU - Brun, F.

AU - Bruno, B.

AU - Bulik, T.

AU - Burger-Scheidlin, C.

AU - Caroff, S.

AU - Casanova, S.

AU - Celic, J.

AU - Cerruti, M.

AU - Chand, T.

AU - Chandra, S.

AU - Chen, A.

AU - Chibueze, J.

AU - Chibueze, O.

AU - Cotter, G.

AU - Dai, S.

AU - Mbarubucyeye, J. D.

AU - Devin, J.

AU - Djannati-Ataï, A.

AU - Dmytriiev, A.

AU - Doroshenko, V.

AU - Egberts, K.

AU - Einecke, S.

AU - Ernenwein, J.-P.

AU - Fegan, S.

AU - Fichet de Clairfontaine, G.

AU - Filipovic, M.

AU - Fontaine, G.

AU - Füßling, M.

AU - Funk, S.

AU - et al, null

PY - 2023/3/1

Y1 - 2023/3/1

N2 - GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE; >100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of Î¦ UL 95 % = 9.7 Ã— 10 âˆ’ 12 erg cm âˆ’ 2 s âˆ’ 1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.

AB - GRB 221009A is the brightest gamma-ray burst (GRB) ever detected. To probe the very-high-energy (VHE; >100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hr after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of Î¦ UL 95 % = 9.7 Ã— 10 âˆ’ 12 erg cm âˆ’ 2 s âˆ’ 1 above E thr = 650 GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the spectral energy distribution occurring above the X-ray band. Compared to the VHE-bright GRB 190829A, the upper limits for GRB 221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB 221009A, effectively ruling out an IC-dominated scenario.

UR - https://hdl.handle.net/1959.7/uws:72994

UR - http://www.scopus.com/inward/record.url?scp=85151509935&partnerID=8YFLogxK

M3 - Article

SN - 2041-8205

VL - 946

JO - Astrophysical Journal Letters

JF - Astrophysical Journal Letters

IS - 1

M1 - L27

ER -

H.E.S.S. follow-up observations of GRB 221009A

Abstract

Bibliographical note

Open Access - Access Right Statement

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