Fermi-GBM Analysis of GRB 221009A

S. Lesage; P. Veres; M. S. Briggs; A. Goldstein; D. Kocevski; E. Burns; C. A. Wilson-Hodge; P. Veres; P. N. Bhat; D. Huppenkothen; C. L. Fryer; R. Hamburg; J. Racusin; E. Bissaldi; W. H. Cleveland; S. Dalessi; C. Fletcher; M. M. Giles; B. A. Hristov; C. M. Hui; B. Mailyan; C. Malacaria; S. Poolakkil; O. J. Roberts; A. von Kienlin; J. Wood; M. Ajello; M. Arimoto; L. Baldini; J. Ballet; M. G. Baring; D. Bastieri; J. Becerra Gonzalez; R. Bellazzini; R. D. Blandford; R. Bonino; P. Bruel; S. Buson; R. A. Cameron; R. Caputo; P. A. Caraveo; E. Cavazzuti; G. Chiaro; N. Cibrario; S. Ciprini; P. Cristarella Orestano; M. Crnogorcevic; A. Cuoco; S. Cutini; F. D’Ammando; S. De Gaetano; N. Di Lalla; L. Di Venere; A. Domínguez; S. J. Fegan; E. C. Ferrara; H. Fleischhack; Y. Fukazawa; S. Funk; P. Fusco; G. Galanti; V. Gammaldi; F. Gargano; C. Gasbarra; D. Gasparrini; S. Germani; F. Giacchino; N. Giglietto; R. Gill; M. Giroletti; J. Granot; D. Green; I. A. Grenier; S. Guiriec; M. Gustafsson; E. Hays; J. W. Hewitt; D. Horan; X. Hou; M. Kuss; L. Latronico; A. Laviron; M. Lemoine-Goumard; J. Li; I. Liodakis; F. Longo; F. Loparco; L. Lorusso; M. N. Lovellette; P. Lubrano; S. Maldera; A. Manfreda; G. Martí-Devesa; M. N. Mazziotta; J. E. McEnery; I. Mereu; M. Meyer; P. F. Michelson; T. Mizuno; M. E. Monzani; A. Morselli; I. V. Moskalenko; M. Negro; E. Nuss; N. Omodei; E. Orlando; J. F. Ormes; D. Paneque; G. Panzarini; M. Persic; M. Pesce-Rollins; R. Pillera; F. Piron; H. Poon; T. A. Porter; G. Principe; S. Rainò; R. Rando; B. Rani; M. Razzano; S. Razzaque; A. Reimer; O. Reimer; F. Ryde; M. Sánchez-Conde; P. M. Saz Parkinson; L. Scotton; D. Serini; C. Sgrò; V. Sharma; E. J. Siskind; G. Spandre; P. Spinelli; H. Tajima; D. F. Torres; J. Valverde; T. Venters; Z. Wadiasingh; K. Wood; G. Zaharijas

Fermi-GBM Analysis of GRB 221009A

S. Lesage
, P. Veres
, M. S. Briggs
, A. Goldstein
, D. Kocevski
, E. Burns
, C. A. Wilson-Hodge
, P. Veres
, P. N. Bhat
, D. Huppenkothen
, C. L. Fryer
, R. Hamburg
, J. Racusin
, E. Bissaldi
, W. H. Cleveland
, S. Dalessi
, C. Fletcher
, M. M. Giles
, B. A. Hristov
, C. M. Hui

B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, G. Chiaro, N. Cibrario, S. Ciprini, P. Cristarella Orestano, M. Crnogorcevic, A. Cuoco, S. Cutini, F. D’Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, S. J. Fegan, E. C. Ferrara, H. Fleischhack, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, C. Gasbarra, D. Gasparrini, S. Germani, F. Giacchino, N. Giglietto, R. Gill, M. Giroletti, J. Granot, D. Green, I. A. Grenier, S. Guiriec, M. Gustafsson, E. Hays, J. W. Hewitt, D. Horan, X. Hou, M. Kuss, L. Latronico, A. Laviron, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, L. Lorusso, M. N. Lovellette, P. Lubrano, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, G. Panzarini, M. Persic, M. Pesce-Rollins, R. Pillera, F. Piron, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, V. Sharma, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, D. F. Torres, J. Valverde, T. Venters, Z. Wadiasingh, K. Wood, G. Zaharijas

University of Alabama in Huntsville
Center for Space Plasma and Aeronomic Research
Universities Space Research Association
NASA Marshall Space Flight Center
Louisiana State University
SRON - Netherlands Institute for Space Research
MST-8, Los Alamos National Laboratory
Université Paris-Saclay
NASA Goddard Space Flight Center
Politecnico di Bari
INFN Sezione di Bari
Jacobs Space Exploration Group
Florida Institute of Technology
International Space Science Institute
Max Planck Institut für Extraterrestrische Physik
Clemson University
Kanazawa University
University of Pisa
CEA/UVSQ/CNRS
Rice University
INFN
University of Padova
Research Unit; CIBERNED and Universidad de La Laguna
Istituto Nazionale di Fisica Nucleare, Sezione di Pisa
Kavli Institute for Particle Astrophysics and Cosmology
INFN Sezione di Torino
University of Turin
University of Würzburg
INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan
Science and Research Directorate
INFN Roma Tor Vergata
University of Perugia
INFN Sezione di Perugia
University of Maryland
INAF Istituto di Radioastronomia
Complutense University
Catholic University of America
Hiroshima University
Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
Universidad Autónoma de Madrid
University of Rome “Tor Vergata”
Instituto de Radioastronomía y Astrofísica
The Open University of Israel
George Washington University
Max-Planck-Institut für Physik
Georg-August-Universität Göttingen
University of North Florida
Yunnan Observatories
Chinese Academy of Sciences
UMR 5797
University of Science and Technology of China
University of Turku
University of Trieste
INFN Sezione di Trieste
The Aerospace Corporation
University of Innsbruck
University of Southern Denmark
Vatican Observatory
Biochemical and Environmental Engineering
Laboratoire Univers et Particules de Montpellier
University of Denver
INAF Osservatorio Astronomico di Padova
Korea Astronomy and Space Science Institute
American University
University of Johannesburg
KTH Royal Institute of Technology
Oskar Klein Centre
University of California at Santa Cruz
NYCB Real-Time Computing Inc.
Nagoya University
Campus UAB
Institut d’Estudis Espacials de Catalunya (IEEC)
Pompeu Fabra University (UPF)
Praxis Inc.
University of Nova Gorica

Résultats de recherche: Contribution à un journal › Article de conférence › Revue par des pairs

1 Citation (Scopus)

Résumé

At 13:16:59.99 UT on October 9th, 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered on gamma-ray burst (GRB) 221009A. This GRB has the highest fluence value GBM has ever detected. The light curve consists of two distinct emission episodes, a single isolated peak with a thermal spectra followed by a longer, extremely bright, multi-pulsed event with a non-thermal spectra. The two main peaks of the second event, from t₀+218 to t₀+276 seconds and t₀+508 to t₀+513 s, had such high photon rates they caused pulse-pile up effects in the GBM detectors. Afterglow emission is detectable in the GBM energy range out to t₀+1467 seconds when the field of view was occulted by Earth. Here we present the key parts of our spectrotemporal analysis for the triggering pulse, prompt emission, and afterglow and the pulse pile-up corrected energetics for the this historically bright event.

langue originale	Anglais
Numéro d'article	882
journal	Proceedings of Science
Volume	444
état	Publié - 27 sept. 2024
Evénement	38th International Cosmic Ray Conference, ICRC 2023 - Nagoya, Japon Durée: 26 juil. 2023 → 3 août 2023

Contient cette citation

Lesage, S., Veres, P., Briggs, M. S., Goldstein, A., Kocevski, D., Burns, E., Wilson-Hodge, C. A., Veres, P., Bhat, P. N., Huppenkothen, D., Fryer, C. L., Hamburg, R., Racusin, J., Bissaldi, E., Cleveland, W. H., Dalessi, S., Fletcher, C., Giles, M. M., Hristov, B. A., ... Zaharijas, G. (2024). Fermi-GBM Analysis of GRB 221009A. Proceedings of Science, 444, Article 882.

@article{89f7985295774d51b61e693cebf0c8b7,

title = "Fermi-GBM Analysis of GRB 221009A",

abstract = "At 13:16:59.99 UT on October 9th, 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered on gamma-ray burst (GRB) 221009A. This GRB has the highest fluence value GBM has ever detected. The light curve consists of two distinct emission episodes, a single isolated peak with a thermal spectra followed by a longer, extremely bright, multi-pulsed event with a non-thermal spectra. The two main peaks of the second event, from t0+218 to t0+276 seconds and t0+508 to t0+513 s, had such high photon rates they caused pulse-pile up effects in the GBM detectors. Afterglow emission is detectable in the GBM energy range out to t0+1467 seconds when the field of view was occulted by Earth. Here we present the key parts of our spectrotemporal analysis for the triggering pulse, prompt emission, and afterglow and the pulse pile-up corrected energetics for the this historically bright event.",

author = "S. Lesage and P. Veres and Briggs, \{M. S.\} and A. Goldstein and D. Kocevski and E. Burns and Wilson-Hodge, \{C. A.\} and P. Veres and Bhat, \{P. N.\} and D. Huppenkothen and Fryer, \{C. L.\} and R. Hamburg and J. Racusin and E. Bissaldi and Cleveland, \{W. H.\} and S. Dalessi and C. Fletcher and Giles, \{M. M.\} and Hristov, \{B. A.\} and Hui, \{C. M.\} and B. Mailyan and C. Malacaria and S. Poolakkil and Roberts, \{O. J.\} and \{von Kienlin\}, A. and J. Wood and M. Ajello and M. Arimoto and L. Baldini and J. Ballet and Baring, \{M. G.\} and D. Bastieri and \{Becerra Gonzalez\}, J. and R. Bellazzini and Blandford, \{R. D.\} and R. Bonino and P. Bruel and S. Buson and Cameron, \{R. A.\} and R. Caputo and Caraveo, \{P. A.\} and E. Cavazzuti and G. Chiaro and N. Cibrario and S. Ciprini and \{Cristarella Orestano\}, P. and M. Crnogorcevic and A. Cuoco and S. Cutini and F. D{\textquoteright}Ammando and \{De Gaetano\}, S. and \{Di Lalla\}, N. and \{Di Venere\}, L. and A. Dom{\'i}nguez and Fegan, \{S. J.\} and Ferrara, \{E. C.\} and H. Fleischhack and Y. Fukazawa and S. Funk and P. Fusco and G. Galanti and V. Gammaldi and F. Gargano and C. Gasbarra and D. Gasparrini and S. Germani and F. Giacchino and N. Giglietto and R. Gill and M. Giroletti and J. Granot and D. Green and Grenier, \{I. A.\} and S. Guiriec and M. Gustafsson and E. Hays and Hewitt, \{J. W.\} and D. Horan and X. Hou and M. Kuss and L. Latronico and A. Laviron and M. Lemoine-Goumard and J. Li and I. Liodakis and F. Longo and F. Loparco and L. Lorusso and Lovellette, \{M. N.\} and P. Lubrano and S. Maldera and A. Manfreda and G. Mart{\'i}-Devesa and Mazziotta, \{M. N.\} and McEnery, \{J. E.\} and I. Mereu and M. Meyer and Michelson, \{P. F.\} and T. Mizuno and Monzani, \{M. E.\} and A. Morselli and Moskalenko, \{I. V.\} and M. Negro and E. Nuss and N. Omodei and E. Orlando and Ormes, \{J. F.\} and D. Paneque and G. Panzarini and M. Persic and M. Pesce-Rollins and R. Pillera and F. Piron and H. Poon and Porter, \{T. A.\} and G. Principe and S. Rain{\`o} and R. Rando and B. Rani and M. Razzano and S. Razzaque and A. Reimer and O. Reimer and F. Ryde and M. S{\'a}nchez-Conde and \{Saz Parkinson\}, \{P. M.\} and L. Scotton and D. Serini and C. Sgr{\`o} and V. Sharma and Siskind, \{E. J.\} and G. Spandre and P. Spinelli and H. Tajima and Torres, \{D. F.\} and J. Valverde and T. Venters and Z. Wadiasingh and K. Wood and G. Zaharijas",

note = "Publisher Copyright: {\textcopyright} Copyright owned by the author(s) under the terms of the Creative Commons.; 38th International Cosmic Ray Conference, ICRC 2023 ; Conference date: 26-07-2023 Through 03-08-2023",

year = "2024",

month = sep,

day = "27",

language = "English",

volume = "444",

journal = "Proceedings of Science",

issn = "1824-8039",

publisher = "Sissa Medialab Srl",

}

Lesage, S, Veres, P, Briggs, MS, Goldstein, A, Kocevski, D, Burns, E, Wilson-Hodge, CA, Veres, P, Bhat, PN, Huppenkothen, D, Fryer, CL, Hamburg, R, Racusin, J, Bissaldi, E, Cleveland, WH, Dalessi, S, Fletcher, C, Giles, MM, Hristov, BA, Hui, CM, Mailyan, B, Malacaria, C, Poolakkil, S, Roberts, OJ, von Kienlin, A, Wood, J, Ajello, M, Arimoto, M, Baldini, L, Ballet, J, Baring, MG, Bastieri, D, Becerra Gonzalez, J, Bellazzini, R, Blandford, RD, Bonino, R, Bruel, P, Buson, S, Cameron, RA, Caputo, R, Caraveo, PA, Cavazzuti, E, Chiaro, G, Cibrario, N, Ciprini, S, Cristarella Orestano, P, Crnogorcevic, M, Cuoco, A, Cutini, S, D’Ammando, F, De Gaetano, S, Di Lalla, N, Di Venere, L, Domínguez, A, Fegan, SJ, Ferrara, EC, Fleischhack, H, Fukazawa, Y, Funk, S, Fusco, P, Galanti, G, Gammaldi, V, Gargano, F, Gasbarra, C, Gasparrini, D, Germani, S, Giacchino, F, Giglietto, N, Gill, R, Giroletti, M, Granot, J, Green, D, Grenier, IA, Guiriec, S, Gustafsson, M, Hays, E, Hewitt, JW, Horan, D, Hou, X, Kuss, M, Latronico, L, Laviron, A, Lemoine-Goumard, M, Li, J, Liodakis, I, Longo, F, Loparco, F, Lorusso, L, Lovellette, MN, Lubrano, P, Maldera, S, Manfreda, A, Martí-Devesa, G, Mazziotta, MN, McEnery, JE, Mereu, I, Meyer, M, Michelson, PF, Mizuno, T, Monzani, ME, Morselli, A, Moskalenko, IV, Negro, M, Nuss, E, Omodei, N, Orlando, E, Ormes, JF, Paneque, D, Panzarini, G, Persic, M, Pesce-Rollins, M, Pillera, R, Piron, F, Poon, H, Porter, TA, Principe, G, Rainò, S, Rando, R, Rani, B, Razzano, M, Razzaque, S, Reimer, A, Reimer, O, Ryde, F, Sánchez-Conde, M, Saz Parkinson, PM, Scotton, L, Serini, D, Sgrò, C, Sharma, V, Siskind, EJ, Spandre, G, Spinelli, P, Tajima, H, Torres, DF, Valverde, J, Venters, T, Wadiasingh, Z, Wood, K & Zaharijas, G 2024, 'Fermi-GBM Analysis of GRB 221009A', Proceedings of Science, VOL. 444, 882.

TY - JOUR

T1 - Fermi-GBM Analysis of GRB 221009A

AU - Lesage, S.

AU - Veres, P.

AU - Briggs, M. S.

AU - Goldstein, A.

AU - Kocevski, D.

AU - Burns, E.

AU - Wilson-Hodge, C. A.

AU - Veres, P.

AU - Bhat, P. N.

AU - Huppenkothen, D.

AU - Fryer, C. L.

AU - Hamburg, R.

AU - Racusin, J.

AU - Bissaldi, E.

AU - Cleveland, W. H.

AU - Dalessi, S.

AU - Fletcher, C.

AU - Giles, M. M.

AU - Hristov, B. A.

AU - Hui, C. M.

AU - Mailyan, B.

AU - Malacaria, C.

AU - Poolakkil, S.

AU - Roberts, O. J.

AU - von Kienlin, A.

AU - Wood, J.

AU - Ajello, M.

AU - Arimoto, M.

AU - Baldini, L.

AU - Ballet, J.

AU - Baring, M. G.

AU - Bastieri, D.

AU - Becerra Gonzalez, J.

AU - Bellazzini, R.

AU - Blandford, R. D.

AU - Bonino, R.

AU - Bruel, P.

AU - Buson, S.

AU - Cameron, R. A.

AU - Caputo, R.

AU - Caraveo, P. A.

AU - Cavazzuti, E.

AU - Chiaro, G.

AU - Cibrario, N.

AU - Ciprini, S.

AU - Cristarella Orestano, P.

AU - Crnogorcevic, M.

AU - Cuoco, A.

AU - Cutini, S.

AU - D’Ammando, F.

AU - De Gaetano, S.

AU - Di Lalla, N.

AU - Di Venere, L.

AU - Domínguez, A.

AU - Fegan, S. J.

AU - Ferrara, E. C.

AU - Fleischhack, H.

AU - Fukazawa, Y.

AU - Funk, S.

AU - Fusco, P.

AU - Galanti, G.

AU - Gammaldi, V.

AU - Gargano, F.

AU - Gasbarra, C.

AU - Gasparrini, D.

AU - Germani, S.

AU - Giacchino, F.

AU - Giglietto, N.

AU - Gill, R.

AU - Giroletti, M.

AU - Granot, J.

AU - Green, D.

AU - Grenier, I. A.

AU - Guiriec, S.

AU - Gustafsson, M.

AU - Hays, E.

AU - Hewitt, J. W.

AU - Horan, D.

AU - Hou, X.

AU - Kuss, M.

AU - Latronico, L.

AU - Laviron, A.

AU - Lemoine-Goumard, M.

AU - Li, J.

AU - Liodakis, I.

AU - Longo, F.

AU - Loparco, F.

AU - Lorusso, L.

AU - Lovellette, M. N.

AU - Lubrano, P.

AU - Maldera, S.

AU - Manfreda, A.

AU - Martí-Devesa, G.

AU - Mazziotta, M. N.

AU - McEnery, J. E.

AU - Mereu, I.

AU - Meyer, M.

AU - Michelson, P. F.

AU - Mizuno, T.

AU - Monzani, M. E.

AU - Morselli, A.

AU - Moskalenko, I. V.

AU - Negro, M.

AU - Nuss, E.

AU - Omodei, N.

AU - Orlando, E.

AU - Ormes, J. F.

AU - Paneque, D.

AU - Panzarini, G.

AU - Persic, M.

AU - Pesce-Rollins, M.

AU - Pillera, R.

AU - Piron, F.

AU - Poon, H.

AU - Porter, T. A.

AU - Principe, G.

AU - Rainò, S.

AU - Rando, R.

AU - Rani, B.

AU - Razzano, M.

AU - Razzaque, S.

AU - Reimer, A.

AU - Reimer, O.

AU - Ryde, F.

AU - Sánchez-Conde, M.

AU - Saz Parkinson, P. M.

AU - Scotton, L.

AU - Serini, D.

AU - Sgrò, C.

AU - Sharma, V.

AU - Siskind, E. J.

AU - Spandre, G.

AU - Spinelli, P.

AU - Tajima, H.

AU - Torres, D. F.

AU - Valverde, J.

AU - Venters, T.

AU - Wadiasingh, Z.

AU - Wood, K.

AU - Zaharijas, G.

PY - 2024/9/27

Y1 - 2024/9/27

N2 - At 13:16:59.99 UT on October 9th, 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered on gamma-ray burst (GRB) 221009A. This GRB has the highest fluence value GBM has ever detected. The light curve consists of two distinct emission episodes, a single isolated peak with a thermal spectra followed by a longer, extremely bright, multi-pulsed event with a non-thermal spectra. The two main peaks of the second event, from t0+218 to t0+276 seconds and t0+508 to t0+513 s, had such high photon rates they caused pulse-pile up effects in the GBM detectors. Afterglow emission is detectable in the GBM energy range out to t0+1467 seconds when the field of view was occulted by Earth. Here we present the key parts of our spectrotemporal analysis for the triggering pulse, prompt emission, and afterglow and the pulse pile-up corrected energetics for the this historically bright event.

AB - At 13:16:59.99 UT on October 9th, 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered on gamma-ray burst (GRB) 221009A. This GRB has the highest fluence value GBM has ever detected. The light curve consists of two distinct emission episodes, a single isolated peak with a thermal spectra followed by a longer, extremely bright, multi-pulsed event with a non-thermal spectra. The two main peaks of the second event, from t0+218 to t0+276 seconds and t0+508 to t0+513 s, had such high photon rates they caused pulse-pile up effects in the GBM detectors. Afterglow emission is detectable in the GBM energy range out to t0+1467 seconds when the field of view was occulted by Earth. Here we present the key parts of our spectrotemporal analysis for the triggering pulse, prompt emission, and afterglow and the pulse pile-up corrected energetics for the this historically bright event.

M3 - Conference article

AN - SCOPUS:85185597755

SN - 1824-8039

VL - 444

JO - Proceedings of Science

JF - Proceedings of Science

M1 - 882

T2 - 38th International Cosmic Ray Conference, ICRC 2023

Y2 - 26 July 2023 through 3 August 2023

ER -

Fermi-GBM Analysis of GRB 221009A

Résumé

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