A 4200-hour HyperFlash and ÉCLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts
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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BibTeX
@misc{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},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2605.18513},
eprint = {2605.18513},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2605.18513},
note = {CC BY 4.0},
}
RIS
TY - UNPB
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 - 2026/10/17
PB - arXiv
DO - 10.48550/arxiv.2605.18513
UR - https://arxiv.org/abs/2605.18513
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 (∼10^40−42 erg) bursts with HyperFlash, which together amount to 4.4 × 10^42 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 ∼2×10^40 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.
ER -