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Search for solar axions produced through the axion-electron coupling $g_{ae}$ using a new GridPix detector at CAST

T0 review · 2 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read This paper reports a search for solar axions at CAST with a seven-chip GridPix detector and finds no signal excess, setting a new upper limit on the product of the axion-electron and axion-photon couplings of $g_{ae}\,g_{a\gamma} <…

desk verdict A careful blinded helioscope search with a new GridPix detector gives a modest best limit, but the quoted mass range is too broad because the massless conversion probability is used for axion masses up to 10 meV. read the letter →

arxiv 2505.05909 v2 pith:IWNGGNUU submitted 2025-05-09 hep-ex

K. Altenmüller , V. Anastassopoulos , S. Arguedas-Cuendis , S. Aune , J. Baier , K. Barth , H. Bräuninger , G. Cantatore
show 56 more authors
F. Caspers J.F. Castel S.A. Çetin F. Christensen C. Cogollos T. Dafni M. Davenport T.A. Decker K. Desch D. Díez-Ibáñez B. Döbrich E. Ferrer-Ribas H. Fischer W. Funk J. Galán J.A. García A. Gardikiotis I. Giomataris J. Golm C.H. Hailey M.D. Hasinoff D.H.H. Hoffmann I.G. Irastorza J. Jacoby A.C. Jakobsen K. Jakovčić J. Kaminski M. Karuza S. Kostoglou C. Krieger J.M. Laurent G. Luzón C. Malbrunot C. Margalejo M. Maroudas L. Miceli H. Mirallas P. Navarro L. Obis A. Özbey K. Özbozduman T. Papaevangelou O. Pérez M.J. Pivovaroff M. Rosu E. Ruiz-Chóliz J. Ruz T. Schiffer S. Schmidt M. Schumann Y.K. Semertzidis S.K. Solanki L. Stewart T. Vafeiadis J.K. Vogel K. Zioutas
This is my paper · ORCID
classification hep-ex
keywords axionaxion-electroncouplinghelioscopeGridPixTimepixsolarbackgroundsuppressionrareeventsearch
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 a search for solar axions using a new seven-chip GridPix detector at the CAST helioscope. Axions produced in the Sun through their coupling to electrons could reconvert into X-rays in the experiment's magnet, and the detector was built to catch those X-rays with very low background. After about 160 hours of solar tracking, no signal excess was seen. The collaboration therefore sets a new upper limit of $g_{ae}\,g_{a\gamma} < 7.35\times10^{-23}\,\mathrm{GeV}^{-1}$ at 95% confidence for axion masses below 10 meV, improving the previous best helioscope limit by about 10%. This demonstrates that GridPix technology, with its single-electron sensitivity and integrated vetoes, is competitive for rare-event searches.

What carries the argument

The central object is the 7-GridPix detector: a gas ionization chamber read out by seven Timepix pixel chips with integrated micromesh amplification grids, giving single-electron sensitivity and per-pixel spatial resolution. The central chip sits at the focal plane of the X-ray telescope, while the six surrounding chips act as an active veto. Background suppression combines a multilayer perceptron classifier trained on simulated X-ray events and real background clusters, a scintillator veto, a longitudinal pulse-shape cut based on the flash ADC, and a pointing veto using the outer chips. The expected axion image comes from a dedicated raytracing simulation, and the final limit is set with an unbinned Bayesian likelihood that is marginalized over nuisance parameters using a Metropolis-Hastings Markov chain Monte Carlo.

What would settle it

Reanalyze the published tracking candidates with the raytraced axion-image region masked out; if the resulting limit moves by more than the quoted uncertainties, the background interpolation is driving the claimed improvement. Conversely, an excess of low-energy clusters whose positions follow the expected axion image would directly falsify the no-signal conclusion.

Watch

Extended reading notes

Core claim

The central claim is that a search for solar axions produced through the axion-electron coupling, using a 7-GridPix detector at CAST, finds no excess above background and therefore sets a new upper limit $g_{ae}\,g_{a\gamma} < 7.35\times10^{-23}\,\mathrm{GeV}^{-1}$ at 95% confidence for axion masses below 10 meV. This improves on the previous CAST bound of $8.1\times10^{-23}\,\mathrm{GeV}^{-1}$ from 2013 by about 10%. The same tracking data also yield a complementary limit on the axion-photon coupling alone, $g_{a\gamma} < 9.0\times10^{-11}\,\mathrm{GeV}^{-1}$, which does not surpass CAST's best axion-photon limit but adds independent model constraints.

Load-bearing premise

The result assumes that the background model built from data taken while the telescope was not tracking the Sun, together with the 86% veto efficiency estimated from chance coincidences, remains valid during the hours the telescope points at the Sun.

Editorial extensions

If this is right

  • The best helioscope constraint on the product $g_{ae}\,g_{a\gamma}$ is now this $7.35\times10^{-23}\,\mathrm{GeV}^{-1}$ limit, replacing the 2013 CAST value as the reference for this coupling product.
  • The analysis pipeline is deliberately generic in the assumed signal spectrum, so the same detector data and background model can be reused for other solar axion production channels without redesigning the limit calculation.
  • The detector's background rate of about $1.06\times10^{-5}\,\mathrm{keV}^{-1}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}$ at roughly 80% signal efficiency in the 0.2-8 keV range puts GridPix on par with the best CAST readout systems for low-background X-ray searches.
  • The derived $g_{a\gamma}$ limit, while not competitive alone with CAST's best axion-photon bound, is already combined with newer Micromegas data in the collaboration's ongoing effort to strengthen helioscope constraints.
  • With only 160 hours of tracking time, the improvement over the previous limit indicates that most of the gain comes from lower background and better signal efficiency rather than longer exposure.

Reading between the lines

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

  • A direct consistency check would be to re-run the limit calculation with the raytraced axion-image region masked out; if the limit changes by much more than the quoted uncertainties, the reported improvement depends on the background interpolation in the signal region.
  • The 86% outer-chip veto efficiency, estimated by bootstrapping random coincidences, suggests that engineering a veto with higher efficiency or a lower random-coincidence rate would directly translate into a stronger $g_{ae}\,g_{a\gamma}$ limit with the same exposure.
  • The ultra-thin silicon-nitride window gives improved transmission below 3 keV, which is exactly where electron-coupled solar axions peak; the same detector concept could be pointed at other low-energy solar or dark-matter signals that are invisible to detectors with thicker windows.
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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 / 5 minor

Summary. The manuscript reports a search for solar axions produced through the axion-electron coupling using a 7-GridPix detector at CAST, with about 160 hours of active solar tracking data from 2017-2018. The analysis uses an MLP-based cluster classifier, scintillator and outer-chip vetoes, a FADC rise-time cut, and a raytracing-based signal spatial template. A Bayesian unbinned likelihood with nuisance parameters yields the central result: g_ae·g_aγ < 7.35×10^-23 GeV^-1 at 95% CL, quoted for axion masses below 10 meV, claimed to improve the previous CAST 2013 bound by about 10%. An ancillary limit g_aγ < 9.0×10^-11 GeV^-1 is also reported.

Significance. If correct, the central limit would be the best helioscope bound on the g_ae–g_aγ product and a valuable demonstration of GridPix technology for future experiments such as IAXO. The analysis has notable strengths: the limit-setting procedure was blinded (expected limits were computed before unblinding), the signal efficiency is calibrated with 55Fe and eight X-ray energies, the telescope response is validated against PANTER measurements, and the analysis framework is open source. However, the quoted limit is stated for a mass range in which the conversion probability used in the signal model is not valid, so the numerical claim as written is not established. The paper is sound in design but needs a substantive revision of the mass dependence before acceptance.

major comments (2)
  1. [§5.1, Eq. (5.2); §6 and Abstract] The signal model in Eq. (5.2) uses the massless conversion probability P_{a→γ,vacuum} without a coherence form factor, yet the abstract and Section 6 quote the limit "for axion masses below 10 meV." For m_a = 10 meV and E ≈ 1 keV, qL = m_a^2 L/(2E) ≈ 2.35, and the factor [sin(qL/2)/(qL/2)]^2 is about 0.62, dropping to about 0.09 at E = 0.5 keV. Because the upper limit on g_ae·g_aγ scales roughly as (signal-weighted P)^{-1/2}, the quoted 7.35×10^-23 GeV^-1 is too strong near the upper end of the claimed mass range; the correction can plausibly exceed the 10% improvement over the CAST 2013 limit. Please provide a mass-dependent exclusion curve, or explicitly restrict the claim to the m_a → 0 limit and state the correspondingly narrow mass range for which the quoted number is valid.
  2. [§5, likelihood definition] The displayed simplification L = e^{-s_tot} ∏_i (1 + s_i/b_i) is not correct as written if the product runs over all bins, because for bins with zero candidates the ratio of Poisson likelihoods contributes e^{-s_i}, not (1 + s_i/b_i). The product should run only over bins containing a candidate. Please correct the derivation or clarify the notation; if the numerical implementation uses the candidate-only product, state this explicitly so the manuscript is self-consistent.
minor comments (5)
  1. [§5.1, Eq. (5.1)] The limit is quoted on the product g_ae·g_aγ, but the prior and posterior in Eq. (5.1) are defined on g_ae with no discussion of how g_aγ is held fixed or marginalized. Please state explicitly how the product limit is obtained from L(g_ae).
  2. [§5.2] The systematic budget lists σ_s, σ_b, and σ_xy, but does not mention an uncertainty on the solar axion flux model from Ref. [15] or on the absolute normalization of the raytracing signal image. Please state whether these are included in σ_s or justify their neglect.
  3. [§4 and Eq. (5.3)] The FADC rise-time cut removes events outside the 1st and 99th percentiles, corresponding to an efficiency of about 98%, but Eq. (5.3) lists only ε_veto and ε_S. The total efficiencies in Table 3 suggest this factor is included; please add it to the formula or explain where it enters.
  4. [§6, Fig. 9] The color scale in Fig. 9 is labeled "Axion flux [a.u.]" but the colorbar ticks are shown in scientific notation with a numeric scale; please clarify the units or remove the numeric ticks to avoid confusion.
  5. [§6] The observed limit is stronger than the median expected limit; reporting the probability of obtaining a limit this strong under the background-only hypothesis would help quantify the significance of the downward fluctuation.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the g_ae·g_aγ limit follows from an external solar axion flux, a standard conversion probability, and detector efficiencies calibrated on real X-ray data, with no signal parameter fitted to the tracking sample.

full rationale

The central claim is a Bayesian upper limit computed from roughly 160 hours of solar-tracking data showing no excess above a background model. The expected signal in Eq. (5.2) is a product of an externally computed solar axion flux, the magnet bore area and tracking time, the standard vacuum conversion probability, measured detection efficiencies, and a raytracing image from a simulation benchmarked against PANTER measurements. None of these factors is adjusted to the tracking candidates to produce the final limit; the only free parameter in the posterior, g_ae, is integrated over with a uniform prior rather than fitted to data. The MLP classifier is trained on simulated X-ray events and background data from outer chips, and the choice of analysis setup was made from expected limits computed with toy candidates before unblinding, as stated in Section 5.3. The veto efficiency is estimated from bootstrapped random coincidences, and the background interpolation is constructed from non-tracking background data; these are inputs to the limit calculation, not quantities whose fitted values are relabeled as the result. The paper's self-references, including [28] for systematic uncertainties and [37] for the analysis code, are not used to replace an independent derivation: the flux and conversion probability are standard physics inputs, and the systematic values are parameter uncertainties rather than the predicted limit itself. The concern raised by the skeptic about the massless conversion probability being quoted up to 10 meV is a question of the validity range of the quoted limit, not a circularity of the derivation chain. No equation reduces to another by construction, and no fitted input is renamed as a prediction; therefore the derivation is self-contained for the purposes of this analysis.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claim rests on standard solar and axion factory inputs, a textbook conversion probability, and detector simulations calibrated to beam tests. No ad hoc entities or fitted parameters are introduced; the two efficiency numbers listed are measured operational quantities.

free parameters (2)
  • MLP software efficiency epsilon_S = 0.952(4) for best setup
    Setpoint chosen to minimize the expected limit; the actual efficiency is calibrated against 55Fe and X-ray-generator data.
  • Outer-chip veto efficiency epsilon_veto = 0.86
    Estimated via bootstrapping random coincidences between center-chip clusters passing the MLP cut and outer-chip clusters; enters the total signal efficiency.
assumptions (5)
  • domain assumption The solar axion flux through the axion-electron coupling (Compton, bremsstrahlung, axio-recombination, axio-deexcitation) is described by Redondo (2013) and used as f(g_ae,E_i) in Eq. 5.2.
    The limit scales with this flux; if the rate or spectrum were wrong, the bound would shift. The calculation is external to this paper.
  • standard math Axion-photon conversion probability in vacuum is P_a->gamma = (g_aγ B L / 2)^2 in natural units.
    Standard helioscope formula; used to compute expected signal. This is textbook physics.
  • domain assumption The X-ray raytracing simulation TrAXer and detector simulation correctly predict the spatial and energy response of the telescope-detector system, validated against PANTER measurements within 2.6% half-power diameter.
    The expected signal image r(x,y) and energy-dependent efficiency come from this simulation; mis-modeling would change sensitivity.
  • domain assumption The MLP event classifier trained on simulated X-ray clusters and outer-chip background generalizes to real tracking data.
    Validated by comparing geometric property distributions of simulated and 55Fe data; the MLP cut is set on simulated data, while efficiency is calibrated with real data.
  • domain assumption A uniform prior on g_ae > 0 in the Bayesian limit is appropriate.
    Statistical convention for upper limits; the result is the 95th percentile of the posterior.

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Cite this review

Pith. "Pith review of Search for solar axions produced through the axion-electron coupling $g_{ae}$ using a new GridPix detector at CAST." pith.science (2026). https://pith.science/paper/IWNGGNUU

@misc{pith2026250505909,
  author       = {Pith},
  title        = {Pith review of: Search for solar axions produced through the axion-electron coupling $g_ae$ using a new GridPix detector at CAST},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/IWNGGNUU}},
  note         = {Machine review of arXiv:2505.05909}
}
abstract

We present a search for solar axions produced through the axion-electron coupling $(g_{ae})$ using data from a novel 7-GridPix detector installed at the CERN Axion Solar Telescope (CAST). The detector, featuring ultra-thin silicon nitride windows and multiple veto systems, collected approximately 160 hours of solar tracking data between 2017-2018. Using machine learning techniques and the veto systems, we achieved a background rate of $1.06\times 10^{-5}\,\text{keV}^{-1}\text{cm}^{-2}\text{s}^{-1}$ at a signal efficiency of about $80\,\%$ in the $0.2$-$8\,\text{keV}$ range. Analysis of the data yielded no significant excess above background, allowing us to set a new upper limit on the product of the axion-electron and axion-photon couplings of $g_{ae}\cdot g_{a\gamma} < 7.35\times 10^{-23}\,\text{GeV}^{-1}$ at $95\,\%$ confidence level. This result improves upon the previous best helioscope limit and demonstrates the potential of GridPix technology for rare event searches. Additionally, we derived a limit on the axion-photon coupling of $g_{a\gamma} < 9.0\times 10^{-11}\,\text{GeV}^{-1}$ at $95\,\%$ CL, which, while not surpassing CAST's best limit, provides complementary constraints on axion models.

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Reference graph

Works this paper leans on

46 extracted references · 37 canonical work pages

  1. [1]

    Weinberg,The u(1) problem,Phys

    S. Weinberg,The u(1) problem,Phys. Rev. D11(1975) 3583

    work page 1975

  2. [2]

    ’t Hooft,Symmetry breaking through bell-jackiw anomalies,Phys

    G. ’t Hooft,Symmetry breaking through bell-jackiw anomalies,Phys. Rev. Lett.37(1976) 8

    work page 1976

  3. [3]

    Hooft,How instantons solve the U(1) problem.,Physics Reports142(1986) 357

    G. Hooft,How instantons solve the U(1) problem.,Physics Reports142(1986) 357

    work page 1986

  4. [4]

    Peccei and H.R

    R.D. Peccei and H.R. Quinn,CPconservation in the presence of pseudoparticles,Phys. Rev. Lett.38(1977) 1440. – 16 – 0 2 4 6 8 10 12 0.1 1 10 100 Energy [keV] Rate [10−5 keV⁻¹cm⁻²s⁻¹] Dataset Background Candidates Figure 10: Comparison of the background and signal rate over the entire chip. No excess in signal visible compared to background model

    work page 1977

  5. [5]

    Peccei and H.R

    R.D. Peccei and H.R. Quinn,Constraints imposed byCPconservation in the presence of pseudoparticles,Phys. Rev. D16(1977) 1791

    1977

  6. [6]

    Weinberg,A new light boson?,Phys

    S. Weinberg,A new light boson?,Phys. Rev. Lett.40(1978) 223

    1978

  7. [7]

    Wilczek,Problem of strong P and T invariance in the presence of instantons,Phys

    F. Wilczek,Problem of strong P and T invariance in the presence of instantons,Phys. Rev. Lett.40(1978) 279

    1978

  8. [8]

    Zioutas, C

    K. Zioutas, C. Aalseth, D. Abriola, F. III, R. Brodzinski, J. Collar et al.,A decommissioned lhc model magnet as an axion telescope,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment425 (1999) 480. [9]CAST Collaborationcollaboration,First results from the CERN axion solar telescop...

    work page 1999

Show all 46 references
  1. [10]

    Irastorza, F

    I. Irastorza, F. Avignone, S. Caspi, J. Carmona, T. Dafni, M. Davenport et al.,Towards a new generation axion helioscope,Journal of Cosmology and Astroparticle Physics2011 (2011) 013

    2011

  2. [11]

    Vogel, F.T

    J.K. Vogel, F.T. Avignone, G. Cantatore, J.M. Carmona, S. Caspi, S.A. Cetin et al.,IAXO - the international axion observatory,1302.3273

    arXiv

  3. [12]

    Armengaud, F.T

    E. Armengaud, F.T. Avignone, M. Betz, P. Brax, P. Brun, G. Cantatore et al.,Conceptual design of the international axion observatory (IAXO),Journal of Instrumentation9(2014) T05002

    2014

  4. [13]

    Zhitnitsky,Possible suppression of axion-hadron interactions,Sov

    A. Zhitnitsky,Possible suppression of axion-hadron interactions,Sov. J. Nucl. Phys. (Engl. Transl.); (United States)31:2(1980) . – 17 –

    1980

  5. [14]

    M. Dine, W. Fischler and M. Srednicki,A simple solution to the strong cp problem with a harmless axion,Physics Letters B104(1981) 199

    1981

  6. [15]

    Redondo,Solar axion flux from the axion-electron coupling,Journal of Cosmology and Astroparticle Physics2013(2013) 008

    J. Redondo,Solar axion flux from the axion-electron coupling,Journal of Cosmology and Astroparticle Physics2013(2013) 008

    2013

  7. [16]

    Berlin, A.J

    A. Berlin, A.J. Millar, T. Trickle and K. Zhou,Physical signatures of fermion-coupled axion dark matter,Journal of High Energy Physics2024(2024)

    2024

  8. [17]

    Aprile, K

    E. Aprile, K. Abe, F. Agostini, S.A. Maouloud, L. Althueser, B. Andrieu et al.,Search for new physics in electronic recoil data from xenonnt,Physical Review Letters129(2022) 161805

    2022

  9. [18]

    Capozzi and G

    F. Capozzi and G. Raffelt,Axion and neutrino bounds improved with new calibrations of the tip of the red-giant branch using geometric distance determinations,Physical Review D102 (2020) 083007

    2020

  10. [19]

    Straniero, C

    O. Straniero, C. Pallanca, E. Dalessandro, I. Domínguez, F.R. Ferraro, M. Giannotti et al., The rgb tip of galactic globular clusters and the revision of the axion-electron coupling bound, Astronomy & Astrophysics644(2020) A166

    2020

  11. [20]

    O’HARE,cajohare/AxionLimits: AxionLimits, July, 2020

    C. O’HARE,cajohare/AxionLimits: AxionLimits, July, 2020. 10.5281/zenodo.3932430

    2020 doi

  12. [21]

    Barth, A

    K. Barth, A. Belov, B. Beltran, H. Bräuninger, J. Carmona, J. Collar et al.,CAST constraints on the axion-electron coupling,Journal of Cosmology and Astroparticle Physics 2013(2013) 010

    2013

  13. [22]

    Llopart, M

    X. Llopart, M. Campbell, R. Dinapoli, D.S. Segundo and E. Pernigotti,Medipix2: A 64-k pixel readout chip with 55- mu;m square elements working in single photon counting mode, IEEE Transactions on Nuclear Science49(2002) 2279

    2002

  14. [23]

    Campbell, M

    M. Campbell, M. Chefdeville, P. Colas, A. Colijn, A. Fornaini, Y. Giomataris et al., Detection of single electrons by means of a micromegas-covered medipix2 pixel cmos readout circuit,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, D...

    2005

  15. [24]

    Chefdeville, P

    M. Chefdeville, P. Colas, Y. Giomataris, H. van der Graaf, E. Heijne, S. van der Putten et al.,An electron-multiplying ‘micromegas’ grid made in silicon wafer post-processing technology,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers,...

    2006

  16. [25]

    van der Graaf,GridPix: An integrated readout system for gaseous detectors with a pixel chip as anode,Nucl

    H. van der Graaf,GridPix: An integrated readout system for gaseous detectors with a pixel chip as anode,Nucl. Instrum. Meth. A580(2007) 1023

    2007

  17. [26]

    Krieger, J

    C. Krieger, J. Kaminski and K. Desch,Ingrid-based x-ray detector for low background searches,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment729(2013) 905

    2013

  18. [27]

    Krieger, J

    C. Krieger, J. Kaminski, M. Lupberger and K. Desch,A gridpix-based x-ray detector for the cast experiment,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment867(2017) 101

    2017

  19. [28]

    Schmidt,Search for solar axions using a 7-GridPix IAXO prototype detector at CAST, Ph.D

    S. Schmidt,Search for solar axions using a 7-GridPix IAXO prototype detector at CAST, Ph.D. thesis, Universitäts-und Landesbibliothek Bonn, 2024

    2024

  20. [29]

    Petre and P.J

    R. Petre and P.J. Serlemitsos,Conical imaging mirrors for high-speed x-ray telescopes,Appl. Opt.24(1985) 1833. – 18 –

    1985

  21. [30]

    Aznar, J.F

    F. Aznar, J.F. Castel, F. Christensen, T. Dafni, T. Decker, E. Ferrer Ribas et al.,A micromegas-based low-background x-ray detector coupled to a slumped-glass telescope for axion research,Journal of Cosmology and Astroparticle Physics2015(2015) 008

    2015

  22. [31]

    Collaboration et al.,New CAST limit on the axion–photon interaction,Nature Physics13 (2017) 584

    C. Collaboration et al.,New CAST limit on the axion–photon interaction,Nature Physics13 (2017) 584

    2017

  23. [32]

    TrAXer - an interactive real-time x-ray raytracer

    S. Schmidt, “TrAXer - an interactive real-time x-ray raytracer.” https://github.com/Vindaar/TrAXer, 2023

    2023

  24. [33]

    Llopart, R

    X. Llopart, R. Ballabriga, M. Campbell, L. Tlustos and W. Wong,Timepix, a 65k programmable pixel readout chip for arrival time, energy and/or photon counting measurements,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and ...

    2007

  25. [34]

    Lupberger,The Pixel-TPC: A feasibility study, Ph.D

    M. Lupberger,The Pixel-TPC: A feasibility study, Ph.D. thesis, Universitäts-und Landesbibliothek Bonn, 2016

    2016

  26. [35]

    TOS - timepix operating software

    “TOS - timepix operating software.”https://github.com/Vindaar/TOS

  27. [36]

    Hierarchical Data Format, version 5

    The HDF Group, “Hierarchical Data Format, version 5.” https://www.hdfgroup.org/HDF5/, 1997-2022

    1997

  28. [37]

    TimepixAnalysis

    S.M. Schmidt, “TimepixAnalysis.”https://github.com/Vindaar/TimepixAnalysis, 2022

    2022

  29. [38]

    Alkhazov,Statistics of electron avalanches and ultimate resolution of proportional counters,Nuclear Instruments and Methods89(1970) 155

    G. Alkhazov,Statistics of electron avalanches and ultimate resolution of proportional counters,Nuclear Instruments and Methods89(1970) 155

    1970

  30. [39]

    Rosenblatt,The perceptron: a probabilistic model for information storage and organization in the brain.,Psychological review65(1958) 386

    F. Rosenblatt,The perceptron: a probabilistic model for information storage and organization in the brain.,Psychological review65(1958) 386

    1958

  31. [40]

    Amari,A theory of adaptive pattern classifiers,IEEE Transactions on Electronic ComputersEC-16(1967) 299

    S. Amari,A theory of adaptive pattern classifiers,IEEE Transactions on Electronic ComputersEC-16(1967) 299

    1967

  32. [41]

    Schmidhuber,Annotated history of modern ai and deep learning,2212.11279

    J. Schmidhuber,Annotated history of modern ai and deep learning,2212.11279

  33. [42]

    Cramér,On the composition of elementary errors,Scandinavian Actuarial Journal1928 (1928) 13

    H. Cramér,On the composition of elementary errors,Scandinavian Actuarial Journal1928 (1928) 13

    1928

  34. [43]

    von Mises,Wahrscheinlichkeit Statistik und Wahrheit, Springer Berlin Heidelberg (1936), 10.1007/978-3-662-41863-5

    R. von Mises,Wahrscheinlichkeit Statistik und Wahrheit, Springer Berlin Heidelberg (1936), 10.1007/978-3-662-41863-5

    1936 doi

  35. [44]

    Anderson,On the distribution of the two-sample cramer-von mises criterion,The Annals of Mathematical Statistics33(1962) 1148

    T.W. Anderson,On the distribution of the two-sample cramer-von mises criterion,The Annals of Mathematical Statistics33(1962) 1148

    1962

  36. [45]

    Metropolis, A.W

    N. Metropolis, A.W. Rosenbluth, M.N. Rosenbluth, A.H. Teller and E. Teller,Equation of state calculations by fast computing machines,The Journal of Chemical Physics21(1953) 1087

    1953

  37. [46]

    Hastings,Monte carlo sampling methods using markov chains and their applications, Biometrika57(1970) 97

    W.K. Hastings,Monte carlo sampling methods using markov chains and their applications, Biometrika57(1970) 97

    1970

  38. [47]

    Altenmüller, V

    K. Altenmüller, V. Anastassopoulos, S. Arguedas-Cuendis, S. Aune, J. Baier, K. Barth et al., New upper limit on the axion-photon coupling with an extended CAST run with a Xe-based micromegas detector,Physical Review Letters133(2024) 221005. – 19 –

    2024

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