Pith. sign in

REVIEW 2 major objections 48 references

A self-triggered radio detector unit achieves operation close to the galactic noise limit through integrated noise modeling and interference rejection.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.3

2026-06-29 10:04 UTC pith:NGD3J6BW

load-bearing objection The paper gives a practical system-level design for self-triggered radio detectors that reaches near galactic noise performance in tests, with a useful indirect noise estimation trick, but the on-site RFI handling needs quantitative checks to confirm the claims. the 2 major comments →

arxiv 2605.28457 v1 pith:NGD3J6BW submitted 2026-05-27 astro-ph.IM

Noise Suppression and Radio Frequency Interference Rejection for Self-Triggered Radio Detectors of Extensive Air Showers

Pengfei Zhang , Xin Xu , Hanrui Wang , Xing Xu , Bohao Duan , Feng Wei , Hongwei Pan , Xishui Tian
show 3 more authors
Yi Zhang Pengxiong Ma Olivier Martineau-Huynh
This is my paper
classification astro-ph.IM
keywords radio detectionextensive air showersRFI rejectiongalactic noiseself-triggered detectorsnoise suppressioncosmic rayselectromagnetic compatibility
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper seeks to demonstrate that radio detectors for extensive air showers can be designed to operate with internal noise low enough that the natural galactic radio background becomes the dominant limit, rather than electronics or local interference. This would matter for building scalable self-triggered arrays that reliably capture rare cosmic ray and neutrino signals without excessive false triggers from anthropogenic radio frequency interference. The work uses a system-level approach that combines sky noise modeling, radio frequency chain noise budgeting, electromagnetic compatibility measures, and both laboratory and field measurements to validate performance. It also presents an indirect method to quantify amplifier noise from measurements at the analog-to-digital converter. The results show the unit can distinguish air shower signals under realistic conditions when the galactic background serves as the reference.

Core claim

By adopting a system-level methodology that integrates sky-noise modeling, RF-chain noise budgeting, electromagnetic compatibility mitigation, and measurement-driven validation, the detector unit operates close to the galactic-noise limit in the core frequency band, allowing extensive air shower radio signals to be distinguished from anthropogenic interference at the system-response level.

What carries the argument

The end-to-end detector design that combines sky-noise modeling, RF-chain noise budgeting, EMC mitigation, and an indirect noise-quantification method using differential internal-noise measurements at the ADC level.

Load-bearing premise

The galactic radio background provides a reliable quantitative reference for judging whether the detector's internal noise is low enough under actual field conditions.

What would settle it

Field measurements in which the detector's internal noise floor exceeds the modeled galactic background by more than a few decibels in the core band, or in which simulated air shower pulses cannot be separated from interference at the trigger level.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Self-triggered operation becomes viable in environments with non-stationary anthropogenic interference.
  • Air shower signals can be identified at the full system response level rather than requiring post-processing.
  • The design methodology can be transferred to other radio arrays for ultra-high-energy particles.
  • Internal noise contributions from the low-noise amplifier can be estimated without direct access to that stage.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Arrays built this way could maintain sensitivity across varying site conditions without frequent hardware redesigns.
  • The same noise budgeting approach might extend to other frequency bands used for cosmic particle detection.
  • Trigger thresholds could be set closer to the theoretical minimum set by the sky, increasing event rates for rare signals.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 0 minor

Summary. The manuscript presents an end-to-end design and experimental characterization of a self-triggered radio detector unit for extensive air showers, optimized for galactic-noise-dominated operation in the classical air-shower radio band. It integrates sky-noise modeling, RF-chain noise budgeting, EMC mitigation, and an indirect ADC-level differential method for LNA noise estimation, with validation via laboratory and on-site measurements claimed to demonstrate operation close to the galactic-noise limit and the ability to distinguish EAS signals from anthropogenic RFI.

Significance. If the quantitative validation holds, the work supplies a practical, system-level methodology for designing scalable self-triggered arrays such as GRAND. It directly tackles the balance between external sky noise, internal detector noise, and non-stationary RFI that limits sensitivity and trigger reliability in radio detection of UHECRs and neutrinos.

major comments (2)
  1. [abstract and on-site measurements section] Abstract and on-site measurements section: the central claim of 'operation close to the galactic-noise limit' and 'measurement-driven validation' supplies no quantitative data, error bars, exclusion criteria, or comparison baselines, so the soundness of the galactic-noise-limited demonstration cannot be assessed from the provided evidence.
  2. [measurement-driven validation and indirect noise-quantification method] Measurement-driven validation and indirect noise-quantification method: the assumption that the galactic radio background provides a stable quantitative reference for separating internal detector noise from external contributions is load-bearing for the validation claim, yet the text does not demonstrate how non-stationary anthropogenic RFI (whose spectral overlap with the core band is not guaranteed to be fully removable by the described EMC mitigation) is excluded; the indirect ADC-level differential method further assumes residual excess after subtraction is attributable only to the amplifier chain rather than unmodeled site or propagation effects.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review. We address each major comment below, agreeing where additional clarity or data presentation is warranted and outlining targeted revisions.

read point-by-point responses

  1. Referee: [abstract and on-site measurements section] Abstract and on-site measurements section: the central claim of 'operation close to the galactic-noise limit' and 'measurement-driven validation' supplies no quantitative data, error bars, exclusion criteria, or comparison baselines, so the soundness of the galactic-noise-limited demonstration cannot be assessed from the provided evidence.

    Authors: We agree that the abstract and on-site measurements section require more explicit quantitative support to allow direct assessment of the claims. While the full manuscript contains the underlying measurement results and model comparisons, these are not summarized with sufficient numerical detail, uncertainties, or baselines in the highlighted locations. In the revised manuscript we will update the abstract with key quantitative outcomes from the validation and expand the on-site section to include error bars, explicit exclusion criteria, and direct comparison baselines against the galactic-noise model. revision: yes

  2. Referee: [measurement-driven validation and indirect noise-quantification method] Measurement-driven validation and indirect noise-quantification method: the assumption that the galactic radio background provides a stable quantitative reference for separating internal detector noise from external contributions is load-bearing for the validation claim, yet the text does not demonstrate how non-stationary anthropogenic RFI (whose spectral overlap with the core band is not guaranteed to be fully removable by the described EMC mitigation) is excluded; the indirect ADC-level differential method further assumes residual excess after subtraction is attributable only to the amplifier chain rather than unmodeled site or propagation effects.

    Authors: The validation procedure selects intervals of low anthropogenic activity through auxiliary monitoring and applies the EMC mitigation described in the manuscript; we will add an explicit subsection detailing the RFI identification and exclusion criteria used for the on-site data. The indirect ADC-level method is cross-checked against laboratory calibrations performed without site propagation effects, and on-site results are compared to the sky-noise model. In revision we will expand the discussion of the method to address potential residual RFI and unmodeled site effects, including quantitative bounds derived from the existing measurements. revision: partial

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The manuscript is an experimental instrumentation paper whose central claims rest on laboratory and on-site measurements that compare detector performance against an external galactic-noise reference. No equations, fitted parameters, or self-citations are presented that would reduce any reported result to a quantity defined by the same result. The validation methodology is therefore independent of its own outputs and remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Only the abstract is available, so the ledger is necessarily incomplete and limited to elements explicitly named in the abstract.

axioms (1)
  • domain assumption Galactic radio background serves as a quantitative reference for assessing internal noise performance
    Invoked when the abstract states that the galactic background is used to assess internal noise and to demonstrate distinction of EAS signals.

pith-pipeline@v0.9.1-grok · 5833 in / 1220 out tokens · 29699 ms · 2026-06-29T10:04:32.758680+00:00 · methodology

0 comments
read the original abstract

Self-triggered radio detection of ultra-high-energy cosmic rays and neutrinos offers a scalable and cost-effective approach for next-generation astroparticle observatories, but remains challenging under realistic radio-frequency interference (RFI) conditions. In the classical air-shower radio band, the achievable sensitivity and trigger reliability are critically limited by the balance between external sky background noise and internal detector-unit noise, as well as by non-stationary anthropogenic interference. In this work, we present an end-to-end design and experimental characterization of a self-triggered radio detector unit explicitly optimized to operate in a galactic-noise-dominated regime. Rather than focusing on a single hardware component or trigger algorithm, we adopt a system-level methodology that coherently integrates sky-noise modeling, RF-chain noise budgeting, electromagnetic compatibility (EMC) mitigation, and measurement-driven validation. By using the galactic radio background as a quantitative reference, we assess the internal noise performance of the detector unit and demonstrate conditions under which extensive air shower (EAS) radio signals can be distinguished from anthropogenic interference at the system-response level. We further introduce an indirect noise-quantification method to estimate the low-noise amplifier contribution within the complete RF chain based on differential internal-noise measurements evaluated at the ADC level. The proposed detector unit is validated through laboratory and on-site measurements, demonstrating operation close to the galactic-noise limit in the core frequency band. These results provide a practical and transferable methodology for the design and deployment of large-scale self-triggered radio arrays such as GRAND.

Figures

Figures reproduced from arXiv: 2605.28457 by Bohao Duan, Feng Wei, Hanrui Wang, Hongwei Pan, Olivier Martineau-Huynh, Pengfei Zhang, Pengxiong Ma, Xing Xu, Xin Xu, Xishui Tian, Yi Zhang.

Figure 1
Figure 1. Figure 1: Principle of high-energy cosmic ray extensive air shower (EAS) detection based on a self-triggered low-frequency radio sparse array. [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Illustration of a typical detection unit: (a) functional module connec [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Schematic diagram of the interference/noise sources, coupling methods, and injection nodes faced by the GP300 unit [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Schematic of the GRANDProto RF Chain Architecture. (a) Electrical [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Galactic noise brightness temperature maps and corresponding power spectral density (PSD). (a)–(h) Sky temperature maps in equatorial coordinates [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Simulation and test results of system noise. (a) Power spectral [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: LNA packaging and shielding strategies developed within the GRAND [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Schematic of the designed low-noise amplifier (LNA), including the input/output matching networks, DC bias network, feedback network, and ESD [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Schematic diagram of metal box packaging test [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Test results of noise contribution of RF chain ( [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Commercial devices for core functional modules in detector units: (a1)–(a2) batteries; (b1)–(b2) charge controllers; (c1)–(c2) GPS antennas; (d1)–(d2) [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Detection units used in the prototype tests (see also the general [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗
Figure 15
Figure 15. Figure 15: Time-domain and frequency-domain test results of RF current on [PITH_FULL_IMAGE:figures/full_fig_p013_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Upgraded components for noise suppression: (a) FEB box (metal [PITH_FULL_IMAGE:figures/full_fig_p015_16.png] view at source ↗
Figure 18
Figure 18. Figure 18: High-impedance low-pass filter (HP-filter) for AM-band suppression: [PITH_FULL_IMAGE:figures/full_fig_p015_18.png] view at source ↗
Figure 17
Figure 17. Figure 17: Typical AM, FM, and Satellite Signal Interference Spectrum [PITH_FULL_IMAGE:figures/full_fig_p015_17.png] view at source ↗
Figure 19
Figure 19. Figure 19: Simulated ADC-level time-domain radio waveforms on the East– [PITH_FULL_IMAGE:figures/full_fig_p017_19.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

48 extracted references · 6 canonical work pages · 1 internal anchor

  1. [1]

    Lu,Modern Astrophysics

    T. Lu,Modern Astrophysics. Beijing, China: Peking Univ. Press, 2014, ISBN 978-7-301-25061-7/O.1019

    2014

  2. [2]

    Measurement and interpretation of UHECR mass composi- tion at the Pierre Auger Observatory,

    E. Mayotte, “Measurement and interpretation of UHECR mass composi- tion at the Pierre Auger Observatory,” arXiv:2507.10292 [astro-ph.HE], 2025

    work page arXiv 2025

  3. [3]

    Radio emission from extensive air showers,

    H. R. Allan, “Radio emission from extensive air showers,” inProgress in Elementary Particles and Cosmic Ray Physics, J. G. Wilson and S. G. Wouthuysen, Eds., vol. 10. Amsterdam, The Netherlands: North- Holland, 1971, pp. 169–302

    1971

  4. [4]

    J. G. Bolton and G. J. Stanley, ”Variable source of radio frequency radiation in the constellation of Cygnus,”Nature, 1948

    1948

  5. [5]

    Abu-Zayyad,et al., ”The surface detector array of the Telescope Array experiment,”Nucl

    T. Abu-Zayyad,et al., ”The surface detector array of the Telescope Array experiment,”Nucl. Instrum. Methods Phys. Res. A, vol. 689, pp. 87–97, Oct. 2012

    2012

  6. [6]

    A population of galaxy-scale jets discovered using LOFAR,

    B. Webster, J. H. Croston, B. Mingo, R. D. Baldi, B. Barkus, G. G ¨urkan, et al., “A population of galaxy-scale jets discovered using LOFAR,” Mon. Not. R. Astron. Soc., vol. 500, no. 4, pp. 4921–4936, 2021

    2021

  7. [7]

    R. M. Almeida, R. Alves Batista, F. Canfora,et al., ”Large-scale and multipolar anisotropies of cosmic rays detected at the Pierre Auger Observatory with energies above 4 EeV ,” 2022. 19

    2022

  8. [8]

    Martineau-Huynh, ”Status of the GRAND project,” arXiv:2507.07260, 2025

    O. Martineau-Huynh, ”Status of the GRAND project,” arXiv:2507.07260, 2025. [Online]. Available: https://arxiv.org/abs/2507.07260

    work page arXiv 2025

  9. [9]

    Wayth, M

    R. Wayth, M. Sokolowski, J. Broderick,et al., ”Engineering devel- opment array 2: Design, performance, and lessons from an SKA-low prototype station,”J. Astronomical Telescopes, Instruments, and Systems, 2021

    2021

  10. [10]

    Seckel, T

    D. Seckel, T. Stanev,et al., ”Neutrinos: The key to ultrahigh energy cosmic rays,”Phys. Rev. Lett., 2005

    2005

  11. [11]

    Kotera, D

    K. Kotera, D. Allard, and A. V . Olinto, ”Cosmogenic neutrinos: Param- eter space and detectability from PeV to ZeV ,”JCAP, no. 10, p. 013, 2010

    2010

  12. [12]

    Heinze, D

    J. Heinze, D. Boncioli, M. Bustamante,et al., ”Cosmogenic neutrinos challenge the cosmic-ray proton dip model,”Astrophys. J., vol. 825, no. 2, p. 122, 2016

    2016

  13. [13]

    ´Alvarez-Mu˜niz,et al., ”The giant radio array for neutrino detection (GRAND): Science and design,”Sci

    J. ´Alvarez-Mu˜niz,et al., ”The giant radio array for neutrino detection (GRAND): Science and design,”Sci. China Phys. Mech. Astron., vol. 63, no. 1, p. 219501, 2020

    2020

  14. [14]

    J. G. Bolton, K. C. Westfold,et al., ”Galactic radiation at radio frequencies. IV . The distribution of radio stars in the galaxy,”Aust. J. Chem., 1951

    1951

  15. [15]

    Danker,Fundamentals of Electromagnetic Compatibility

    B. Danker,Fundamentals of Electromagnetic Compatibility. Bicon Lab- oratories, 2004

    2004

  16. [16]

    Chiong,et al., ”Low-noise amplifier for next-generation radio astronomy telescopes: Review of the state-of-the-art cryogenic LNAs in the most challenging applications,”IEEE Microw

    C.-C. Chiong,et al., ”Low-noise amplifier for next-generation radio astronomy telescopes: Review of the state-of-the-art cryogenic LNAs in the most challenging applications,”IEEE Microw. Mag., vol. 23, no. 1, pp. 31–47, 2021

    2021

  17. [17]

    R. J. Cameron, C. M. Kudsia, and R. R. Mansour,Microwave Filters for Communication Systems: Fundamentals, Design, and Applications. Hoboken, NJ, USA: Wiley, 2018

    2018

  18. [18]

    A. R. Offringa,et al., ”A LOFAR RFI detection pipeline and its first results,” arXiv:1007.2089, 2010. [Online]. Available: https://arxiv.org/abs/1007.2089

    work page internal anchor Pith review Pith/arXiv arXiv 2089

  19. [19]

    Kampert and A

    K.-H. Kampert and A. A. Watson, ”Extensive air showers and ultra high- energy cosmic rays: A historical review,”Eur. Phys. J. H, vol. 37, no. 3, pp. 359–412, 2012

    2012

  20. [20]

    A. L. Cummings,et al., ”Modeling the optical Cherenkov signals by cosmic ray extensive air showers directly observed from suborbital and orbital altitudes,”Phys. Rev. D, vol. 104, no. 6, p. 063029, 2021

    2021

  21. [21]

    G. A. Askaryan,et al., ”Excess negative charge of electron-photon shower and the coherent radiation originating from it,”J. Phys. Soc. Jpn., 1962

    1962

  22. [22]

    F. D. Kahn and I. Lerche, ”Radiation from cosmic ray air showers,” Proc. R. Soc. Lond. A, 1966

    1966

  23. [23]

    Huege, ”Theory and simulations of air shower radio emission,” in Proc

    T. Huege, ”Theory and simulations of air shower radio emission,” in Proc. AIP Conf., vol. 1535, no. 1, pp. 121–127, 2013

    2013

  24. [24]

    Zhang, T

    K. Zhang, T. Huege, R. Koirala,et al., ”Electric field recon- struction with three polarizations for the radio detection of ultra- high energy particles,” arXiv:2501.12614, 2025. [Online]. Available: https://arxiv.org/abs/2501.12614

    work page arXiv 2025

  25. [25]

    Guelfand,et al., ”Reconstruction of inclined extensive air showers using radio signals: From arrival times and amplitudes to direction and energy,”Astropart

    M. Guelfand,et al., ”Reconstruction of inclined extensive air showers using radio signals: From arrival times and amplitudes to direction and energy,”Astropart. Phys., vol. 17, p. 103120, 2025

    2025

  26. [26]

    Schl ¨uter and T

    F. Schl ¨uter and T. Huege, ”Signal model and event reconstruction for the radio detection of inclined air showers,”JCAP, vol. 2023, no. 01, p. 008, 2023

    2023

  27. [27]

    Long-term calibration and validation of stability of the Auger Engineering Radio Array using the diffuse Galactic radio emission,

    A. Halim,et al., “Long-term calibration and validation of stability of the Auger Engineering Radio Array using the diffuse Galactic radio emission,”J. Instrum., vol. 20, no. 12, p. P12017, 2025

    2025

  28. [28]

    Charrier, K

    D. Charrier, K. D. de Vries, Q. Gou,et al., ”Autonomous radio detection of air showers with the TREND50 antenna array,”Astropart. Phys., vol. 110, pp. 15–29, 2019

    2019

  29. [29]

    Chiche, K

    S. Chiche, K. Kotera, O. Martineau-Huynh,et al., ”Polarisation signa- tures in radio for inclined cosmic-ray induced air-shower identification,” Astropart. Phys., vol. 139, p. 102696, 2022

    2022

  30. [30]

    S. W. Barwick, D. Z. Besson, A. Burgman,et al., ”Radio detection of air showers with the ARIANNA experiment on the Ross Ice Shelf,” Astropart. Phys., vol. 90, pp. 50–68, 2017

    2017

  31. [31]

    Platania, C

    P. Platania, C. Burigana, D. Maino,et al., ”Full sky study of diffuse galactic emission at decimeter wavelengths,”Astron. Astrophys., vol. 410, no. 3, pp. 847–863, 2003

    2003

  32. [32]

    H. V . Cane, ”Spectra of the non-thermal radio radiation from the galactic polar regions,”Mon. Not. R. Astron. Soc., vol. 189, no. 3, pp. 465–478, 1979

    1979

  33. [33]

    ”Towards the Giant Radio Array for Neutrino Detection (GRAND): The GRANDProto300 and GRAND@Auger prototypes,” in preparation

  34. [34]

    Alves Batista,et al., ”GRANDlib: A simulation pipeline for the Giant Radio Array for Neutrino Detection (GRAND),”Comput

    R. Alves Batista,et al., ”GRANDlib: A simulation pipeline for the Giant Radio Array for Neutrino Detection (GRAND),”Comput. Phys. Commun., vol. 308, p. 109461, 2025

    2025

  35. [35]

    Polisensky, ”LFmap: A low frequency sky map generating program,” LWA Memo Ser., vol

    E. Polisensky, ”LFmap: A low frequency sky map generating program,” LWA Memo Ser., vol. 111, p. 515, 2007

    2007

  36. [36]

    Uncertainty of ADC Random Noise Estimates Obtained With the IEEE 1057 Standard Test,

    F. M. Alegreia and A. C. Serra, “Uncertainty of ADC Random Noise Estimates Obtained With the IEEE 1057 Standard Test,”IEEE Trans. Instrum. Meas., vol. 54, no. 1, pp. 110–116, Feb. 2005

    2005

  37. [37]

    Histogram Measurement of ADC Nonlinearities Using Sine Waves,

    J. J. Blair, “Histogram Measurement of ADC Nonlinearities Using Sine Waves,”IEEE Trans. Instrum. Meas., vol. 43, no. 3, pp. 373–383, Jun. 1994

    1994

  38. [38]

    Clery, ”Neutrino astronomers set biggest traps ever for messen- gers from cosmic accelerators,”Science, Aug

    D. Clery, ”Neutrino astronomers set biggest traps ever for messen- gers from cosmic accelerators,”Science, Aug. 21, 2025. [Online]. Available: https://www.science.org/content/article/neutrino-astronomers- set-biggest-traps-ever-messengers-cosmic-accelerators

    2025

  39. [39]

    Probe Characterization for Electromagnetic Near-Field Studies,

    S. Jarrix, T. Dubois, R. Adam, P. Nouvel, B. Azais, and D. Gasquet, “Probe Characterization for Electromagnetic Near-Field Studies,”IEEE Trans. Instrum. Meas., vol. 59, no. 2, pp. 292–300, Feb. 2010

    2010

  40. [40]

    Group-Delay Measurement of Frequency- Converting Devices Using a Comb Generator,

    J. Scott and M. Hoy, “Group-Delay Measurement of Frequency- Converting Devices Using a Comb Generator,”IEEE Trans. Instrum. Meas., vol. 59, no. 11, pp. 3012–3017, Nov. 2010

    2010

  41. [41]

    Alvarez-Mu ˜niz, W

    J. Alvarez-Mu ˜niz, W. R. Carvalho Jr., and E. Zas, ”Monte Carlo simulations of radio pulses in atmospheric showers using ZHAireS,” Astropart. Phys., vol. 35, no. 6, pp. 325–341, 2012

    2012

  42. [42]

    Thamizharasan and N

    V . Thamizharasan and N. Kasthuri, ”FPGA implementation of high per- formance digital FIR filter design using a hybrid adder and multiplier,” Int. J. Electron., vol. 110, no. 4, pp. 587–607, 2023

    2023

  43. [43]

    L. Tan, J. Jiang, and L. Wang, ”Pole-radius-varying IIR notch filter with transient suppression,”IEEE Trans. Instrum. Meas., vol. 61, no. 6, pp. 1684–1691, 2012

    2012

  44. [44]

    Automatic Power Frequency Rejection Instrumentation for Nonintrusive Frequency Signature Tracking,

    K. Lee, “Automatic Power Frequency Rejection Instrumentation for Nonintrusive Frequency Signature Tracking,”IEEE Trans. Instrum. Meas., vol. 70, 2021

    2021

  45. [45]

    Digital Q-Varying Notch IIR Filter With Transient Suppression,

    J. Piskorowski, “Digital Q-Varying Notch IIR Filter With Transient Suppression,”IEEE Trans. Instrum. Meas., vol. 59, no. 4, pp. 866–872, Apr. 2010

    2010

  46. [46]

    Correa and J

    P. Correa and J. K ¨ohler, ”NUTRIG: Development of a novel radio self-trigger for GRAND,” arXiv:2507.04339, 2025. [Online]. Available: https://arxiv.org/abs/2507.04339

    work page arXiv 2025

  47. [47]

    B. Hare, O. Scholten, S. Buitink,et al., ”Characteristics of recoil leaders as observed by LOFAR,”Phys. Rev. D, 2023

    2023

  48. [48]

    Benoit-L ´evy, Z

    A. Benoit-L ´evy, Z. Lai, O. Macias,et al., ”Denoising radio pulses from air showers using machine-learning methods,” arXiv:2507.06688, 2025. [Online]. Available: https://arxiv.org/abs/2507.06688

    work page arXiv 2025