GRB 241030A: a bright afterglow challenging forward shock emission

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dc.contributor.authorDucoin, J.-G.
dc.contributor.authorPellouin, C.
dc.contributor.authorAivazyan, V.
dc.contributor.authorAkl, D.
dc.contributor.authorAlvarez, F.
dc.contributor.authorAndrade, C.
dc.contributor.authorAngulo, C.
dc.contributor.authorAntier, S.
dc.contributor.authorAtteia, J.-L.
dc.contributor.authorBasa, S.
dc.contributor.authorBecerra, R. L.
dc.contributor.authorBenkhaldoun, Z.
dc.contributor.authorBissaldi, E.
dc.contributor.authorBreeveld, A.
dc.contributor.authorBruin, E. de
dc.contributor.authorBurns, E.
dc.contributor.authorButler, N. R.
dc.contributor.authorCoughlin, M. W.
dc.contributor.authorDaigne, F.
dc.contributor.authorDietrich, T.
dc.contributor.authorDornic, D.
dc.contributor.authorDouzet, C.
dc.contributor.authorLaz, T. du
dc.contributor.authorDuverne, P.-A.
dc.contributor.authorEggenstein, H. B.
dc.contributor.authorElhosseiny, E.
dc.contributor.authorEsamdin, A.
dc.contributor.authorEvans, P. A.
dc.contributor.authorFernández, J. F. Agüí
dc.contributor.authorFerro, M.
dc.contributor.authorFortin, F.
dc.contributor.authorFreeberg, M.
dc.contributor.authorGarcía-García, L.
dc.contributor.authorGill, R.
dc.contributor.authorGlobus, N.
dc.contributor.authorGuessoum, N.
dc.contributor.authorHamed, G. M.
dc.contributor.authorHello, P.
dc.contributor.authorAirasca, A. Holzmann
dc.contributor.authorHu, D. F.
dc.contributor.authorHussenot-Desenonges, T.
dc.contributor.authorInasaridze, R.
dc.contributor.authorIskandar, A.
dc.contributor.authorJiang, S. Q.
dc.contributor.authorJin, C. C.
dc.contributor.authorKaeouach, A.
dc.contributor.authorKarpov, S.
dc.contributor.authorKlingler, Noel
dc.contributor.authorKlotz, A.
dc.contributor.authorKochiashvili, N.
dc.contributor.authorKoehn, H.
dc.contributor.authorKneip, R.
dc.contributor.authorKvernadze, T.
dc.contributor.authorCalloch, A. Le
dc.contributor.authorLee, W. H.
dc.contributor.authorLekic, A.
dc.contributor.authorLiang, Y. F.
dc.contributor.authorLimonta, C.
dc.contributor.authorLiu, J.
dc.contributor.authorLópez, K. Ocelotl C.
dc.contributor.authorLópez-Cámara, D.
dc.contributor.authorMabrouk, R. H.
dc.contributor.authorMagnani, F.
dc.contributor.authorMao, J.
dc.contributor.authorMašek, M.
dc.contributor.authorMéndez, E. Moreno
dc.contributor.authorMihov, B. M.
dc.contributor.authorMolham, M.
dc.contributor.authorNoysena, K.
dc.contributor.authorOdeh, M.
dc.contributor.authorOmodei, N.
dc.contributor.authorPeng, H.
dc.contributor.authorPereyra, M.
dc.contributor.authorPillas, M.
dc.contributor.authorPillera, R.
dc.contributor.authorPradier, T.
dc.contributor.authorRajabov, Y.
dc.contributor.authorRakotondrainibe, N. A.
dc.contributor.authorSchneider, B.
dc.contributor.authorSerrau, M.
dc.contributor.authorSlavcheva-Mihova, L.
dc.contributor.authorSokoliuk, O.
dc.contributor.authorSun, H.
dc.contributor.authorTakey, A.
dc.contributor.authorTanasan, M.
dc.contributor.authorTinyanont, K. S.
dc.contributor.authorTurpin, D.
dc.contributor.authorPostigo, A. de Ugarte
dc.contributor.authorWang, B. T.
dc.contributor.authorWang, L. T.
dc.contributor.authorWang, X. F.
dc.contributor.authorWang, Z. M.
dc.contributor.authorWatson, A. M.
dc.contributor.authorWu, H. Z.
dc.contributor.authorWu, Q. Y.
dc.contributor.authorXu, J. J.
dc.contributor.authorYan, Y. S.
dc.contributor.authorYang, H. N.
dc.contributor.authorYuan, W.
dc.contributor.authorZhao, H. S.
dc.date.accessioned2026-04-06T18:35:32Z
dc.date.issued2026-03-19
dc.description.abstractGamma-Ray Burst GRB 241030A (z = 1.411) exhibited a bright afterglow (similar to GRB 221009A), detected across gamma-ray, X-ray, UV, and optical bands, providing a probe of GRB afterglow physics. We compiled multi-wavelength observations spanning from a minute to a week after the prompt emission, processing the data through a unified photometry pipeline. We analysed the observations both analytically and using Bayesian inference with two independent models. Our models assume that the afterglow emission arises from the strong forward shock of a laterally structured jet, with possible contributions from synchrotron self-Compton (SSC) scatterings. Our models reproduce X-ray to optical data, favouring a jet propagating into a constant-density interstellar medium, with a viewing angle within the jet core. However, both analyses require parameter values that are extreme compared to expectations from standard theory. In particular, our results imply extremely energetic jets despite regular prompt energy, leading to a very inefficient prompt emission. Furthermore, the jets are inefficient at accelerating particles, with low electron and magnetic energy fractions, leading to significant SSC emission. Our analyses indicate that the jets have large opening angles and propagate in high-density media. If the afterglow is indeed powered by radiation emitted behind a strong forward shock, our results place GRB 241030A within a sub-class of GRBs characterised by extreme kinetic energies, large jet opening angles, and very low prompt emission efficiencies, with strong SSC radiation. These predictions are difficult to reconcile with typical expectations from other GRBs. We therefore suggest that the afterglow of GRB 241030A is not solely powered by forward shock emission.
dc.description.sponsorshipM.W. C. acknowledges support from the National Science Foundation with grant numbers PHY-2117997, PHY-2308862 and PHY-2409481. N. G. acknowledges the support of the Simons Foundation (MP-SCMPS-00001470, N. G.). H. K. acknowledges funding from the European Union (ERC, SMArt, 101076369). N. J. K. acknowledges support by NASA under award number 80GSFC24M0006. J. M. acknowledges support by the National Key R&D Program of China (2023YFE0101200), Natural Science Foundation of China 12393813, and the Yunnan Revitalization Talent Support Program (YunLing Scholar Project). C. P. acknowledges support by consolidator ERC grant 818899 (JetNS). A.M. W. acknowledges support by UNAM/DGAPA project IN109224. The NRIAG team acknowledges financial support from the Egyptian Science, Technology & Innovation Funding Authority (STDF) under grant number 45779. B.M. M. and L. S.-M. acknowledge support from the infrastructure purchased/renovated under the National Roadmap for Research Infrastructure (2020-2027), financially coordinated by the Ministry of Education and Science of Republic of Bulgaria (agreement D01-326/04.12.2023). M. M. and S. K. acknowledge support by MEYS (Czech Republic) under the projects Czech Republic MEYS LM2023032, LM2023047, and CZ.02.01.01/00/22_008/0004632. The COLIBRÍ team acknowledges support of the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams. AbAO team acknowledges Shota Rustaveli National Science Foundation of Georgia (SRNSFG, grant FR-24-7713). E. B., A. H. A., N. O. and R. P. acknowledge support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K.A. Wallenberg Foundation, the Swedish Research Council and the National Space Board (Sweden). This work is also supported in the operations phase from INAF (Italy), and CNES (France) is also gratefully acknowledged. This work was performed in part under the DOE Contract DEAC02-76SF00515. This work is partly based on data obtained with the CFH/Megacam instrument, and the ACME is thanked for providing necessary time for this work. COLIBRÍ received support from the French government under the France 2030 investment plan, as part of the Initiative d’Excellence d’Aix-Marseille Université-A*MIDEX through (ANR-11-LABX-0060 - OCEVU) and (AMX-19-IET008 - IPhU), from LabEx FOCUS (ANR-11-LABX-0013), From Centre National d’Etudes Spatiale (CNES) and from CSAAINSU-CNRS support program, and in Mexico from UNAM (Secretaria Administrativa, Coordinacion de la Investigacion Cient?fica, Instituto de Astronom?a and PAPIIT grant IN105921), and SECIHTI/CONACyT (277901, Ciencias de Frontera 1046632 and Laboratorios Nacionales). This work is also partly based on data obtained with the instrument OSIRIS, built by a Consortium led by the Instituto de Astrofísica de Canarias in collaboration with the Instituto de Astronomía of the Universidad Autónoma de México. OSIRIS was funded by GRANTECAN and the National Plan of Astronomy and Astrophysics of the Spanish Government. This work is finally based on observations made with the Thai Robotic Telescope under program ID TRTC12A_001, which is operated by the National Astronomical Research Institute of Thailand (Public Organization). CFH and Skyportal are part of a project that has received funding from the European Union’s Horizon Europe Research and innovation programme under Grant Agreement No 101131928. This project is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-FranceHawai’i Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawai’i. C. D. acknowledges funding from the European Union’s Horizon Europe Research and Innovation Programme under Grant Agreement No 101131928 (ACME project). The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.
dc.description.urihttp://arxiv.org/abs/2603.18956
dc.format.extent20 pages
dc.genrejournal articles
dc.genrepreprints
dc.identifierdoi:10.13016/m2phv6-5166
dc.identifier.urihttps://doi.org/10.48550/arXiv.2603.18956
dc.identifier.urihttp://hdl.handle.net/11603/42400
dc.language.isoen
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Faculty Collection
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.rightsAttribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.en
dc.subjectAstrophysics - High Energy Astrophysical Phenomena
dc.titleGRB 241030A: a bright afterglow challenging forward shock emission
dc.typeText

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