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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

A 4200-hour HyperFlash and ÉCLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts

  • O S Ould-Boukattine1,2
  • A J Cooper3
  • A M Cook4,5,2
  • J W T Hessels4,5,2,1
  • D M Hewitt2
  • J Huang4,5
  • I Cognard6,7
  • T J Dijkema1,8
  • M P Gawroński9
  • W Herrmann10
  • F Kirsten11,1
  • A Moroianu2
5 more authors
  • Z Pleunis2,1
  • W Puchalska9
  • S Ranguin2
  • M P Snelders1,2
  • T Telkamp8
11 affiliations
  1. 1ASTRON, Netherlands Institute for Radio Astronomy , Oude Hoogeveensedijk 4, 7991 PD Dwingeloo ,
  2. 2Anton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, 1098 XH, Amsterdam ,
  3. 3Astrophysics, The University of Oxford , Keble Road, Oxford, OX1 3RH ,
  4. 4Trottier Space Institute, McGill University , 3550 rue University, Montréal, QC H3A 2A7 ,
  5. 5McGill University Department of Physics, , 3600 rue University, Montréal, QC H3A 2T8 ,
  6. 6Station de Radioastronomie de Nançay, Observatoire de Paris , PSL University, CNRS, Université d’Orléans, F-18330 Nançay ,
  7. 7Laboratoire de Physique et Chimie de l’Environnement et de l’Espace LPC2E UMR7328, Université d’Orléans , CNRS, F-45071 Orléans ,
  8. 8CAMRAS Dwingeloo Radio Telescope Foundation , Oude Hoogeveensedijk 4, 7991 PD Dwingeloo ,
  9. 9Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University , Grudziadzka 5, 87-100 Toruń ,
  10. 10Astropeiler Stockert e.V. , Astropeiler 1-4, 53902 Bad Münstereifel ,
  11. 11Chalmers University of Technology Department of Physics and Astronomy, , Onsala Space Observatory, 439 92, Onsala ,
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Abstract

Hyperactive repeaters provide a unique window into the evolving environments and energy budgets of fast radio burst (FRB) sources, though they may not be representative of the FRB population in general. High-cadence observations are key to capturing the rarest and most energetic bursts, which occur only once per hundreds to thousands of hours. Here we present an unprecedented 4, 200-hour observing campaign targeting FRB 20240114A as part of the HyperFlash and ÉCLAT FRB monitoring programs. Over 806 days, we detected 178 high-energy (∼1040 − 42 erg) bursts with HyperFlash, which together amount to 4.4 × 1042 erg of released radio energy (assuming isotropic emission and 1-GHz emission bandwidth). The cumulative energy of the HyperFlash bursts is about twice that of ∼11, 000 lower-energy bursts detected with FAST, emphasising the significant role that the highest-energy bursts play in depleting the central engine’s stored energy. In fact, the single most brilliant burst from our sample, which we term the STROOP, contributes roughly 1/3 of all the energy we measure, and is at the maximum energy seen in studies of both repeating and apparently one-off FRBs alike. We also find a break in the burst energy distribution at ∼2 × 1040 erg and a linear dispersion measure (DM) increase of +0.96 ± 0.06 pc cm−3 over a period of 318 days. We discuss these findings in the context of a magnetar source model and highlight comparisons with the energetics of intermediate and giant X-ray/γ-ray flares from Galactic sources.

Versions

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Cite

BibTeXRIS
BibTeX
@article{ouldboukattine20264200hour,
  title = {{A 4200-hour HyperFlash and ÉCLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts}},
  author = {O S Ould-Boukattine and A J Cooper and A M Cook and J W T Hessels and D M Hewitt and J Huang and I Cognard and T J Dijkema and M P Gawroński and W Herrmann and F Kirsten and A Moroianu and Z Pleunis and W Puchalska and S Ranguin and M P Snelders and T Telkamp},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1957},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1957/8931749},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - A 4200-hour HyperFlash and ÉCLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts
AU  - O S Ould-Boukattine
AU  - A J Cooper
AU  - A M Cook
AU  - J W T Hessels
AU  - D M Hewitt
AU  - J Huang
AU  - I Cognard
AU  - T J Dijkema
AU  - M P Gawroński
AU  - W Herrmann
AU  - F Kirsten
AU  - A Moroianu
AU  - Z Pleunis
AU  - W Puchalska
AU  - S Ranguin
AU  - M P Snelders
AU  - T Telkamp
PY  - 2026
DA  - 2026/10/16
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1957
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag1957/8931749
AB  - Hyperactive repeaters provide a unique window into the evolving environments and energy budgets of fast radio burst (FRB) sources, though they may not be representative of the FRB population in general. High-cadence observations are key to capturing the rarest and most energetic bursts, which occur only once per hundreds to thousands of hours. Here we present an unprecedented 4, 200-hour observing campaign targeting FRB 20240114A as part of the HyperFlash and ÉCLAT FRB monitoring programs. Over 806 days, we detected 178 high-energy (∼1040 − 42 erg) bursts with HyperFlash, which together amount to 4.4 × 1042 erg of released radio energy (assuming isotropic emission and 1-GHz emission bandwidth). The cumulative energy of the HyperFlash bursts is about twice that of ∼11, 000 lower-energy bursts detected with FAST, emphasising the significant role that the highest-energy bursts play in depleting the central engine’s stored energy. In fact, the single most brilliant burst from our sample, which we term the STROOP, contributes roughly 1/3 of all the energy we measure, and is at the maximum energy seen in studies of both repeating and apparently one-off FRBs alike. We also find a break in the burst energy distribution at ∼2 × 1040 erg and a linear dispersion measure (DM) increase of +0.96 ± 0.06 pc cm−3 over a period of 318 days. We discuss these findings in the context of a magnetar source model and highlight comparisons with the energetics of intermediate and giant X-ray/γ-ray flares from Galactic sources.
SN  - 0035-8711
SN  - 1365-2966
ER  -