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REVIEW 2 major objections 8 minor 89 references

H.E.S.S. programme searching for VHE gamma rays associated with FRBs

T0 review · 2 major / 8 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read This paper reports that H.E.S.S. observations from 2015 to 2022 found no significant very-high-energy gamma-ray emission from any fast radio burst source, and sets 99% confidence upper limits on the VHE luminosity of nine localized…

desk verdict Solid null results and a useful compilation, but treat the 10^44–10^48 erg/s luminosity range as assumption-dependent, not a robust physical bound. read the letter →

arxiv 2507.02143 v1 pith:TQU5R7KB submitted 2025-07-02 astro-ph.HE

F. Aharonian , A. Archaryya , J. Aschersleben , H. Ashkar , M. Backes , V. Barbosa. Martins , R. Batzofin , Y. Becherini
show 122 more authors
D. Berge K. Bernlöhr M. Böttcher C. Boisson J. Bolmont M. de. Bony. de. Lavergne J. Borowska F. Bradascio R. Brose A. Brown F. Brun B. Bruno C. Burger-Scheidlin S. Casanova J. Celic M. Cerruti T. Chand S. Chandra A. Chen J. Chibueze O. Chibueze J. Damascene. Mbarubucyeye J. de. Assis. Scarpin A. Djannati-Ataï J. Djuvsland A. Dmytriiev K. Egberts S. Einecke J.-P. Ernenwein C. Escañuela. Nieves M. Filipovic G. Fontaine S. Funk S. Gabici J.F. Glicenstein J. Glombitza G. Grolleron B. Hess W. Hofmann T. L. Holch M. Holler D. Horns Zhiqiu. Huang A. Jaitly M. Jamrozy F. Jankowsky I. Jung-Richardt E. Kasai K. Katarzyński D. Kerszberg R. Khatoon B. Khélifi W. Kluźniak Nu. Komin K. Kosack D. Kostunin A. Kundu R.G. Lang S. Le. Stum A. Lemière M. Lemoine-Goumard J.-P. Lenain A. Luashvili J. Mackey D. Malyshev V. Marandon R. Marx A. Mehta M. Meyer A. Mitchell R. Moderski M.O. Moghadam E. Moulin M. de. Naurois J. Niemiec P. O'Brien L. Olivera-Nieto E. de. Ona. Wilhelmi M. Ostrowski S. Panny M. Panter R.D. Parsons U. Pensec S. Pita G. Pühlhofer M. Punch A. Quirrenbach S. Ravikularaman M. Regeard O. Reimer H. Ren B. Reville F. Rieger G. Rowell B. Rudak K. Sabri V. Sahakian H. Salzmann A. Santangelo M. Sasaki J. Schäfer F. Schüssler H.M. Schutte J.N.S. Shapopi A. Sharma S. Spencer {L}. Stawarz R. Steenkamp S. Steinmassl C. Steppa T. Takahashi T. Tanaka M. Tsirou C. van. Eldik M. Vecchi C. Venter T. Wach S.J. Wagner A. Wierzcholska A.A. Zdziarski A. Zech N. Żywucka
This is my paper
classification astro-ph.HE
keywords fastradioburstsveryhighenergygammaraysH.E.S.S.magnetarsupperlimitsmultiwavelengthcampaignsextragalacticbackgroundlighttransientastronomy
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper reports the results of the H.E.S.S. programme searching for very-high-energy (VHE) gamma-ray counterparts to fast radio bursts (FRBs) over 2015 to 2022. Across target-of-opportunity follow-ups of radio and X-ray triggers, magnetar observations, and coordinated multiwavelength campaigns with radio and X-ray facilities, no significant VHE emission was found. For nine FRBs with well-localized host galaxies at redshifts 0.11 to 0.49, the 99% confidence upper limits on VHE luminosity fall between $10^{44}$ and $10^{48}$ erg s$^{-1}$ after correcting for extragalactic background light absorption. These bounds bear on the leading idea that FRBs come from magnetars, since they constrain persistent and afterglow VHE emission from FRB source regions across timescales from hours to years.

What carries the argument

The central mechanism is the H.E.S.S. target-of-opportunity and multiwavelength observation programme combined with a standard upper-limit pipeline. The instrument is an array of five imaging atmospheric Cherenkov telescopes (CT1$-$4 plus the larger CT5) sensitive from about 30 GeV to 100 TeV; events are reconstructed with a maximum-likelihood gamma-hadron separation method, background is estimated with the reflected-background technique, and 99% confidence flux upper limits are computed under an assumed $E^{-2}$ power-law spectrum. To turn flux limits into luminosity limits, the paper corrects for extragalactic background light absorption using the adopted EBL model at each host-galaxy redshift. The ToO system automatically filters radio alerts (signal-to-noise above 10, human-vetted alerts, dispersion measure below 1000 pc cm$^{-3}$) and can begin observations within hours, which is what allows afterglow constraints on hour-to-year timescales.

What would settle it

Search the same 2015 to 2022 H.E.S.S. data at the nine localized FRB positions using a different background-estimation method, such as ring background instead of reflected background, and a different assumed spectral index; a greater-than-$5\sigma$ excess in any field would contradict the claim that no significant VHE emission was detected.

Watch

Extended reading notes

Core claim

The paper's central claim is that H.E.S.S. detected no significant VHE gamma-ray emission from any FRB source, magnetar, or campaign field observed between 2015 and 2022. The programme covered three target-of-opportunity follow-ups (FRB 20150215, FRB 20150418A, and FRB 20190806A), two magnetars (SGR 1935+2154 and SGR 1830$-$0645), the 2019 Deeper Wider Faster campaign, and two MeerKAT campaigns targeting repeating and non-repeating FRBs. For the nine localized extragalactic FRBs, the authors convert 99% confidence flux upper limits into luminosity upper limits assuming an $E^{-2}$ spectrum and EBL attenuation, yielding limits in the range $10^{44}$ to $10^{48}$ erg s$^{-1}$. They also report no millisecond-scale TeV pulses coincident with X-ray bursts from SGR 1935+2154 and set steady flux limits such as $\Phi_\gamma(E>420\,\mathrm{GeV}) < 1.27 \times 10^{-12}$ erg cm$^{-2}$ s$^{-1}$. The conclusion is that any persistent VHE emission in the FRB regions is fainter than these bounds, and any afterglow emission during the observed windows was absent.

Load-bearing premise

The luminosity limits assume any VHE emission follows an $E^{-2}$ power-law spectrum and that the extragalactic background light model used for absorption corrections is accurate; if the true spectrum is much harder or softer, or the EBL opacity differs at these redshifts, the quoted $10^{44}$ to $10^{48}$ erg s$^{-1}$ range would shift, though the non-detection itself would stand.

Editorial extensions

If this is right

  • Persistent very-high-energy emission from the regions of the nine localized FRBs is ruled out above $10^{44}$ to $10^{48}$ erg s$^{-1}$, depending on source redshift.
  • The absence of a TeV afterglow from FRB 20190806A starting 4.5 hours after the burst, and from FRB 20150418A starting 14.5 hours after the burst, constrains afterglow models on hour-to-day timescales.
  • For SGR 1935+2154, no steady or millisecond-timescale TeV emission accompanied the X-ray bursting phase, tightening limits on magnetar high-energy emission.
  • Simultaneous MeerKAT, H.E.S.S., and Swift campaigns found no radio, X-ray, or VHE emission during the observing windows, including no persistent radio counterpart.
  • The nine luminosity upper limits are comparable to Fermi-LAT limits and sit several orders of magnitude above the roughly $10^{39}$ erg s$^{-1}$ persistent luminosities some models expect at 1 TeV, so current data cannot yet test those predictions.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A stacked analysis of the nine localized fields, which the paper does not present, could push the combined limit below the individual $10^{44}$ erg s$^{-1}$ floor, leaving room for fainter collective emission.
  • Prompt TeV emission during the few-millisecond radio burst itself remains essentially untested by these observations, since the constraints apply to persistent and afterglow emission, so a magnetar model that emits TeV only during the burst is not ruled out.
  • Because predicted persistent VHE luminosities are several orders of magnitude below these limits, the non-detections are consistent with most current theory, and the decisive test may come from future Cherenkov observatories with lower energy thresholds and an order of magnitude better sensitivity.
  • The emphasis on southern-sky coverage means that repeating FRBs visible only to northern radio arrays remain less constrained in the VHE band, so the northern-hemisphere telescopes are the natural complement for those sources.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 8 minor

Summary. This paper describes the H.E.S.S. FRB programme from 2015 to 2022. It reports Target-of-Opportunity observations of FRB 20150215A, FRB 20150418A, and FRB 20190806A, observations of the magnetars SGR 1935+2154 and SGR 1830-0645, and multi-wavelength campaigns with the Deeper Wider Faster programme and with MeerKAT/Swift. No significant very-high-energy gamma-ray emission is detected in any observation. Using the H.E.S.S. 99% C.L. integral flux upper limits, the paper derives VHE luminosity upper limits for the extragalactic FRB positions listed in Table 3, after correcting for EBL absorption and assuming an E^-2 spectrum, and reports a range of 10^44 to 10^48 erg/s. These limits are compared with Fermi-LAT, X-ray, and theoretical predictions.

Significance. The non-detection and upper limits provide useful observational constraints from the only southern-hemisphere imaging atmospheric Cherenkov telescope with an active FRB follow-up programme. The paper has archival value as a unified summary of the H.E.S.S. FRB observations and offers a homogeneous compilation of luminosity limits in Table 3. The analysis methods (Rolke, Feldman-Cousins, Li and Ma) are standard, the flux limits refer to previously published papers, and the non-detection result itself is robust. The principal new quantitative claim, however, is the 10^44 to 10^48 erg/s luminosity range, and that range is conditional on spectral-shape and EBL-model assumptions that are not stated precisely and whose systematic impact is not quantified; this tempers the significance of the central claim.

major comments (2)
  1. [Section 5, Table 3] The luminosity upper limits in Table 3 are the central quantitative result, but the EBL model used for the absorption correction is not stated anywhere in the paper, and the sensitivity of L_VHE,host to the assumed intrinsic photon index (E^-2) is not discussed. At the redshifts of this sample, the EBL optical depth is large and strongly energy dependent above ~100 GeV; different EBL models (e.g., Dominguez et al. 2011 vs Franceschini and Rodighiero 2017) and harder or softer intrinsic spectra can change the inferred luminosity by an amount that is not negligible compared with the reported 10^44 to 10^48 erg/s span. I ask the authors to specify the EBL model, to recompute the limits for at least two EBL models and two spectral indices (e.g., gamma = 1.5 and gamma = 2.5), and to either quote the resulting systematic spread or state explicitly in the abstract and in the Table 3 caption that the luminosity range assumes a particular model.
  2. [Section 3.2, Table 3, Section 5] FRB 20190806A is listed in Table 3 with z < 0.32 derived from its dispersion measure and has no host-galaxy association; it is not a localized FRB in the same sense as the other entries with spectroscopic host redshifts. Including it in the statement in Section 5 that nine localized FRBs have redshifts between 0.11 and 0.49, and in the corresponding abstract sentence, overstates the sample by one source. Please either remove it from the summary statistics or clearly mark its redshift as a dispersion-measure upper limit and its luminosity limit as distance-dependent.
minor comments (8)
  1. [Section 5] The text contains a duplicated and malformed sentence: 'ranging beetween 10 44 erg s^-1 and 1048 erg s^-1' appears twice, and 'raging' should be 'ranging'.
  2. [Section 3.2] The first paragraph refers to 'FRB 20190816' where the source under discussion is FRB 20190806A; the object name should be made consistent.
  3. [Section 3.1] 'Feldman Cousin method' should be 'Feldman-Cousins method'.
  4. [Section 3.3] The spacing in 'F AST' is a typo for FAST, and the magnetar is referred to inconsistently as both 'SGR J1935+2154' and 'SGR 1935+2154'; a single naming convention should be used.
  5. [References] References [81] and [91] cite the same paper (Principe et al. 2023); the duplicate should be removed or merged.
  6. [Table 3 caption] The caption is ungrammatical in the final sentence ('The chance association ... are taken from the works cited in Ref. LVHE,host constrains ...'); it should be rewritten to separate the chance-association note from the definition of L_VHE,host.
  7. [Section 4.2 and Figure 5] The text states that the FRB 20171019A flux upper limits were calculated at 95% C.L., while the Figure 5 caption refers to 99% C.L. differential upper limits; the confidence level for the MeerKAT-campaign limits should be stated consistently.
  8. [Section 2] The claim that H.E.S.S. has 'more than 20 times greater energy flux sensitivity' than Fermi-LAT at 1 GeV lacks a specific citation and should be referenced or qualified.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the non-detection and upper limits are direct observational products, compared against independent external models and instruments; stated spectral and EBL assumptions are conventions, not fitted inputs.

full rationale

The paper's central claim is an observational null result: no significant VHE gamma-ray emission was found in H.E.S.S. observations of FRB fields, magnetars, or ToO follow-ups from 2015 to 2022, and 99% C.L. upper limits on VHE luminosity fall between 10^44 and 10^48 erg/s for nine localized FRBs. The derivation chain runs from H.E.S.S. event data through likelihood reconstruction, reflected-background estimation, and Rolke upper limits under an assumed E^-2 spectrum, followed by an EBL correction using the external Domínguez et al. (2011) model and host-galaxy redshifts from the literature. None of these inputs is defined in terms of the reported luminosity limits, and no parameter is fitted to the FRB sample and then renamed as a prediction. The E^-2 assumption is explicitly stated as a convention because the intrinsic spectrum is unknown, not because it was tuned to produce the quoted range. The EBL model and redshifts are externally sourced. The comparison values from Murase et al., Lyubarsky, Fermi-LAT, Konus-Wind, and X-ray observations are independent external benchmarks. The self-citations to earlier H.E.S.S. papers report the same observations, analysis methods, or instrument descriptions; they are data provenance and technical references rather than load-bearing theoretical premises. The luminosity range is convention- and model-dependent in the sense that a different spectral index or EBL model would shift the derived limits, but this is a robustness caveat, not circularity. The non-detection itself does not depend on those choices. The paper is self-contained as an observational upper-limit study, so no circular step is present.

Assumptions & free parameters 1 free parameters · 3 assumptions · 0 invented entities

The only hand-chosen parameter is the spectral index; the external assumptions are the EBL model and literature host associations. No new physical entities are introduced.

free parameters (1)
  • Assumed photon spectral index = 2 (E^-2, assumed)
    Assumed to convert H.E.S.S. count upper limits into integral flux and luminosity limits (Section 2). Not fitted; a different index would shift the limits.
assumptions (3)
  • domain assumption Extragalactic background light attenuation follows the Domínguez et al. (2011) model.
    Used in Section 5 to correct flux upper limits to rest-frame VHE luminosity limits in Table 3.
  • domain assumption The host galaxy associations and redshifts for the nine extragalactic FRBs are correct as reported in the cited literature.
    The luminosity limits in Table 3 place each FRB at its host redshift; chance association probabilities up to 0.026 mean a wrong association would invalidate that source's limit.
  • standard math Standard Poisson background statistics (Rolke, Feldman-Cousins, Li and Ma) apply to the H.E.S.S. event counts.
    Used for all upper limits and significance maps in Sections 2, 3 and 4.

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Cite this review

Pith. "Pith review of H.E.S.S. programme searching for VHE gamma rays associated with FRBs." pith.science (2026). https://pith.science/paper/TQU5R7KB

@misc{pith2026250702143,
  author       = {Pith},
  title        = {Pith review of: H.E.S.S. programme searching for VHE gamma rays associated with FRBs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TQU5R7KB}},
  note         = {Machine review of arXiv:2507.02143}
}
abstract

Fast Radio Bursts (FRBs) are highly energetic, extremely short-lived bursts of radio flashes. Despite extensive research, the exact cause of these outbursts remains speculative. The high luminosity, short duration, and high dispersion measure of these events suggest they result from extreme, high-energy extragalactic sources, such as highly magnetized and rapidly spinning neutron stars known as magnetars. The number of detected FRBs, including repeating ones, has grown rapidly in recent years. Except for FRB 20200428D, and FRB-like radio burst that is associated to Galactic magnetar SGR 1935+2154, no multi-wavelength counterpart to any FRB has been detected yet. The High Energy Stereoscopic System (H.E.S.S.) telescope has developed a {program} to follow up FRBs searching for their gamma-ray counterparts, helping to uncover the nature of FRBs and FRB sources. This paper provides an overview of the searches for FRB sources conducted by H.E.S.S., including follow-up observations and simultaneous multi-wavelength campaigns with radio and X-ray observatories. Among the FRB sources observed by H.E.S.S., nine are localized with redshifts ranging between 0.11 and 0.492 from 2015 to 2022. No significant very high energy (VHE) emission was detected during these observations. We report constraints on the VHE luminosity ranging from $10^{44}$ erg s$^{-1}$ and $10^{48}$ erg s$^{-1}$, placing limits on the FRB's region persistent VHE emission and potential FRB afterglow emission across timescales from hours to years.

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