pith. sign in

arxiv: 2606.05320 · v1 · pith:3LJJWYGVnew · submitted 2026-06-03 · ✦ hep-ph · astro-ph.CO· astro-ph.HE· hep-ex

Gravitational Wave Imprints of a High-Quality Axion and the Origin of Flavor Hierarchies

Pith reviewed 2026-06-28 05:13 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HEhep-ex
keywords axionflavor symmetriesgravitational wavescosmic stringsFroggatt-Nielsen mechanismdark matterstrong CP problemPeccei-Quinn symmetry
0
0 comments X

The pith

Gauged flavor symmetries protect axions from Planck effects and generate a plateau-valley gravitational wave spectrum from cosmic strings.

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

The paper establishes that gauged abelian flavor symmetries invoked to explain fermion mass hierarchies via the Froggatt-Nielsen mechanism also shield the Peccei-Quinn axion from dangerous Planck-suppressed operators. This produces an accidental high-quality flavored axion with unit domain wall number. The same setup predicts both low-energy flavor-changing neutral currents such as K to pi a decays and stochastic gravitational waves sourced by networks of flavonic and axionic cosmic strings, with global axionic strings additionally able to account for dark matter. The resulting GW spectrum exhibits a characteristic plateau-valley structure that serves as a distinctive observational signature.

Core claim

Constructions with gauged U(1)_F flavor symmetries shield the axion from Planck-suppressed operators, yielding an accidental high-quality flavored axion with unit domain wall number. These predict flavor-changing neutral currents at high flavor scales and stochastic gravitational waves from the evolution and decay of gauged flavonic and axionic cosmic-string networks, while global axionic strings can radiate axions to match the observed dark matter abundance. The resulting plateau-valley structure in the GW spectrum provides a distinctive probe of high-quality flavored axion dark matter models complementary to low-energy flavor experiments.

What carries the argument

Gauged flavonic and axionic cosmic-string networks whose evolution and decay source stochastic gravitational waves with a plateau-valley spectrum.

If this is right

  • High flavor scales Lambda_FN greater than or equal to f_a lead to observable flavor-changing neutral currents such as K to pi a decays.
  • Global axionic strings efficiently radiate axions that can account for the full dark matter relic density.
  • The plateau-valley feature in the GW spectrum arises specifically from the combined flavonic and axionic string networks.
  • The GW signal provides a probe independent of and complementary to searches for flavor violation at low energies.

Where Pith is reading between the lines

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

  • Future GW observatories sensitive to the relevant frequency bands could directly test the cosmic string contribution without requiring flavor violation signals.
  • The unit domain wall number condition may restrict the possible flavor symmetry charge assignments that simultaneously solve strong CP and flavor problems.
  • If axions constitute dark matter via string radiation, the same models predict correlated signals in both GW detectors and flavor experiments.

Load-bearing premise

Gauged abelian flavor symmetries U(1)_F naturally shield the axion from Planck-suppressed operators while yielding an accidental high-quality flavored axion with unit domain wall number.

What would settle it

A measured stochastic gravitational wave spectrum from cosmic strings that lacks the predicted plateau-valley structure, or the absence of K to pi a decays at the expected rates for Lambda_FN greater than or equal to f_a.

Figures

Figures reproduced from arXiv: 2606.05320 by K.S. Babu, Sai Charan Chandrasekar, Sudip Jana, Sudip Manna.

Figure 1
Figure 1. Figure 1: The characteristic plateau-valley GW spectra for different values of axion decay constant [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Detection prospects for the corresponding axion decay constant ( [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Summary of the model parameter space showing the regions allowed by current experimental and theoretical con [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
read the original abstract

Axions, arising from an anomalous global Peccei-Quinn symmetry $U(1)_{\text{PQ}}$, offer a compelling solution to the strong CP problem but are vulnerable to Planck-suppressed operators. Gauged abelian flavor symmetries $U(1)_F$, invoked to explain the flavor hierarchies via the Froggatt-Nielsen mechanism, can naturally shield the axion from such effects, yielding an accidental high-quality flavored axion with unit domain wall number. Such constructions predict two complementary signatures: (i) flavor-changing neutral currents from $K\to\pi a$ decays, typically associated with high flavor scales $\Lambda_{\text{FN}}\gtrsim f_a$, and (ii) stochastic Gravitational Waves (GWs) sourced by the evolution and decay of gauged flavonic and axionic cosmic-string networks. In addition, global axionic strings can efficiently radiate axions, potentially accounting for the observed dark matter relic abundance. We show that the resulting characteristic plateau--valley structure in the GW spectrum provides a distinctive and powerful probe of high-quality flavored axion dark matter models, complementary to low-energy flavor experiments.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 2 minor

Summary. The manuscript argues that gauged U(1)_F abelian flavor symmetries, introduced via the Froggatt-Nielsen mechanism to explain fermion mass hierarchies, can simultaneously protect an axion from Planck-suppressed operators. This yields an accidental high-quality axion with N_DW=1 whose associated flavonic and axionic string networks produce a characteristic plateau-valley structure in the stochastic gravitational-wave spectrum; the same construction also allows global axionic strings to radiate axions that may account for the dark-matter relic density. These features are presented as complementary probes to low-energy flavor processes such as K oπa decays.

Significance. If the central derivation holds, the work supplies a concrete, observationally distinctive link between flavor model-building and gravitational-wave phenomenology. The predicted spectral feature is falsifiable with future GW observatories and does not rely on post-hoc parameter tuning according to the abstract; this strengthens the case for the model as a unified explanation of flavor hierarchies, axion quality, and dark matter.

minor comments (2)
  1. The abstract states that the plateau-valley structure 'provides a distinctive and powerful probe,' but the manuscript should explicitly state the frequency range and amplitude scaling in terms of the string tension and network parameters to allow direct comparison with projected sensitivities of LISA, ET, or pulsar-timing arrays.
  2. Notation for the flavor scale Λ_FN versus the axion decay constant f_a should be clarified in the introductory section; the relation Λ_FN ≳ f_a is mentioned but its precise impact on the domain-wall number and string network evolution is not immediately transparent from the abstract alone.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for the positive assessment of our manuscript, the clear summary of its main results, and the recommendation for minor revision. No major comments appear in the report.

Circularity Check

0 steps flagged

No significant circularity; derivation chain is self-contained against external benchmarks

full rationale

The provided abstract and reader's summary present the central claim as a standard logical chain (gauged U(1)_F flavor symmetry → accidental high-quality axion with N_DW=1 → string network evolution → distinctive GW plateau-valley spectrum) without any quoted equations, fitted parameters, or self-citations that reduce a prediction to an input by construction. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citations appear in the visible material. The GW signature is framed as a derived consequence of string network dynamics, which are independently modeled in the broader literature, making the result falsifiable outside the paper's own choices. This is the normal case of an honest non-finding.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities can be extracted or audited from the provided text.

pith-pipeline@v0.9.1-grok · 5753 in / 1198 out tokens · 30624 ms · 2026-06-28T05:13:36.181728+00:00 · methodology

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

57 extracted references · 20 linked inside Pith

  1. [1]

    resonant leptogenesis

    and an SM scalar singletSby the addition of the flavon fieldX. The role of theSfield in the DFSZ model is to avoid the Weinberg-Wilczek weak scale axion [8, 9] ruled out by ex- periments. This generalization integrates seamlessly with the FN mechanism using two Higgs doublets for the up- type, down-type quarks, plus charged lepton couplings, respectively....

  2. [2]

    axionic”global strings and Type-fstrings as“flavonic

    points corresponding to variousrvalues, which are highlighted in Fig. 3. We consider a concrete scenario with (n, k) = (3,1 +), h u = 4, h d =−2/3, q X = 1 fixingq S = −13/9 =l/mfrom Eq. (4) as a simple and illustrative example and analyze the production of GWs in the com- ing section, while contrasting it with the axion flavor ob- servables of the curren...

  3. [3]

    MINIMAL FLAVOR UNIFICATION VIA MULTIGENERATIONAL PECCEI-QUINN SYMMETRY,

    A. Davidson and K. C. Wali, “MINIMAL FLAVOR UNIFICATION VIA MULTIGENERATIONAL PECCEI-QUINN SYMMETRY,”Phys. Rev. Lett.48 (1982) 11

  4. [4]

    Axions and Family Symmetry Breaking,

    F. Wilczek, “Axions and Family Symmetry Breaking,” Phys. Rev. Lett.49(1982) 1549–1552

  5. [5]

    Family symmetry, gravity, and the strong CP problem,

    K. S. Babu and S. M. Barr, “Family symmetry, gravity, and the strong CP problem,”Phys. Lett. B300(1993) 367–372,arXiv:hep-ph/9212219

  6. [6]

    Flaxion: a minimal extension to solve puzzles in the standard model,

    Y. Ema, K. Hamaguchi, T. Moroi, and K. Nakayama, “Flaxion: a minimal extension to solve puzzles in the standard model,”JHEP01(2017) 096, arXiv:1612.05492 [hep-ph]

  7. [7]

    Minimal axion model from flavor,

    L. Calibbi, F. Goertz, D. Redigolo, R. Ziegler, and J. Zupan, “Minimal axion model from flavor,”Phys. 9 Rev. D95no. 9, (2017) 095009,arXiv:1612.08040 [hep-ph]

  8. [8]

    Fermion Mass Hierarchy and a High Quality Axion From Gauged U(1) Flavor Symmetry,

    K. S. Babu, S. C. Chandrasekar, and Z. Tavartkiladze, “Fermion Mass Hierarchy and a High Quality Axion From Gauged U(1) Flavor Symmetry,” (Feb, 2026) , arXiv:2602.24253 [hep-ph]

  9. [9]

    CP Conservation in the Presence of Instantons,

    R. D. Peccei and H. R. Quinn, “CP Conservation in the Presence of Instantons,”Phys. Rev. Lett.38(1977) 1440–1443

  10. [10]

    A New Light Boson?,

    S. Weinberg, “A New Light Boson?,”Phys. Rev. Lett. 40(1978) 223–226

  11. [11]

    Problem of StrongPandTInvariance in the Presence of Instantons,

    F. Wilczek, “Problem of StrongPandTInvariance in the Presence of Instantons,”Phys. Rev. Lett.40(1978) 279–282

  12. [12]

    Chiral Dynamics in the Large n Limit,

    P. Di Vecchia and G. Veneziano, “Chiral Dynamics in the Large n Limit,”Nucl. Phys. B171(1980) 253–272

  13. [13]

    Chiral Estimate of the Electric Dipole Moment of the Neutron in Quantum Chromodynamics,

    R. J. Crewther, P. Di Vecchia, G. Veneziano, and E. Witten, “Chiral Estimate of the Electric Dipole Moment of the Neutron in Quantum Chromodynamics,”Phys. Lett. B88(1979) 123. [Erratum: Phys.Lett.B 91, 487 (1980)]

  14. [14]

    Measurement of the Permanent Electric Dipole Moment of the Neutron,

    C. Abelet al., “Measurement of the Permanent Electric Dipole Moment of the Neutron,”Phys. Rev. Lett.124 no. 8, (2020) 081803,arXiv:2001.11966 [hep-ex]

  15. [15]

    Planck scale physics and the Peccei-Quinn mechanism,

    M. Kamionkowski and J. March-Russell, “Planck scale physics and the Peccei-Quinn mechanism,”Phys. Lett. B282(1992) 137–141,arXiv:hep-th/9202003

  16. [16]

    Solutions to the strong CP problem in a world with gravity,

    R. Holman, S. D. H. Hsu, T. W. Kephart, E. W. Kolb, R. Watkins, and L. M. Widrow, “Solutions to the strong CP problem in a world with gravity,”Phys. Lett. B282(1992) 132–136,arXiv:hep-ph/9203206

  17. [17]

    Planck scale corrections to axion models,

    S. M. Barr and D. Seckel, “Planck scale corrections to axion models,”Phys. Rev. D46(1992) 539–549

  18. [18]

    Accidental Peccei-Quinn Symmetry From Gauged U(1) and a High Quality Axion,

    K. S. Babu, B. Dutta, and R. N. Mohapatra, “Accidental Peccei-Quinn Symmetry From Gauged U(1) and a High Quality Axion,” (12, 2024) , arXiv:2412.21157 [hep-ph]

  19. [19]

    Hierarchy of Quark Masses, Cabibbo Angles and CP Violation,

    C. D. Froggatt and H. B. Nielsen, “Hierarchy of Quark Masses, Cabibbo Angles and CP Violation,”Nucl. Phys. B147(1979) 277–298

  20. [20]

    Topology of Cosmic Domains and Strings,

    T. W. B. Kibble, “Topology of Cosmic Domains and Strings,”J. Phys. A9(1976) 1387–1398

  21. [21]

    Vilenkin and E

    A. Vilenkin and E. P. S. Shellard,Cosmic Strings and Other Topological Defects. Cambridge University Press, 7, 2000

  22. [22]

    Gravitational radiation from cosmic strings,

    A. Vilenkin, “Gravitational radiation from cosmic strings,”Phys. Lett. B107(1981) 47–50

  23. [23]

    Radiation From Vacuum Strings and Domain Walls,

    T. Vachaspati, A. E. Everett, and A. Vilenkin, “Radiation From Vacuum Strings and Domain Walls,” Phys. Rev. D30(1984) 2046

  24. [24]

    From U(1)×U(1) symmetry breaking to Majoron cosmology: Insights from NANOGrav 15-year data,

    T. Ghosh, K. Loho, and S. Manna, “From U(1)×U(1) symmetry breaking to Majoron cosmology: Insights from NANOGrav 15-year data,”Phys. Rev. D113 no. 4, (2026) 043036,arXiv:2507.04342 [hep-ph]. [23]LISACollaboration, P. Amaro-Seoaneet al., “Laser Interferometer Space Antenna,”arXiv:1702.00786 [astro-ph.IM]

  25. [25]

    Unveiling the gravitational universe atµ-Hz frequencies,

    A. Sesanaet al., “Unveiling the gravitational universe atµ-Hz frequencies,”Exper. Astron.51no. 3, (2021) 1333–1383,arXiv:1908.11391 [astro-ph.IM]

  26. [26]

    Laser interferometry for the big bang observer,

    G. M. Harry, P. Fritschel, D. A. Shaddock, W. Folkner, and E. S. Phinney, “Laser interferometry for the big bang observer,”Class. Quant. Grav.23(2006) 4887–4894. [Erratum: Class.Quant.Grav. 23, 7361 (2006)]

  27. [27]

    Current status of space gravitational wave antenna DECIGO and B-DECIGO,

    S. Kawamuraet al., “Current status of space gravitational wave antenna DECIGO and B-DECIGO,” PTEP2021no. 5, (2021) 05A105,arXiv:2006.13545 [gr-qc]

  28. [28]

    Detecting a gravitational-wave background with next-generation space interferometers,

    H. Kudoh, A. Taruya, T. Hiramatsu, and Y. Himemoto, “Detecting a gravitational-wave background with next-generation space interferometers,”Phys. Rev. D 73(2006) 064006,arXiv:gr-qc/0511145

  29. [29]

    Pushing towards the ET sensitivity using ’conventional’ technology,

    S. Hild, S. Chelkowski, and A. Freise, “Pushing towards the ET sensitivity using ’conventional’ technology,” arXiv:0810.0604 [gr-qc]. [29]AEDGECollaboration, Y. A. El-Neajet al., “AEDGE: Atomic Experiment for Dark Matter and Gravity Exploration in Space,”EPJ Quant. Technol.7 (2020) 6,arXiv:1908.00802 [gr-qc]. [30]LIGO ScientificCollaboration, B. P. Abbott...

  30. [30]

    On Possible Suppression of the Axion Hadron Interactions. (In Russian),

    A. R. Zhitnitsky, “On Possible Suppression of the Axion Hadron Interactions. (In Russian),”Sov. J. Nucl. Phys. 31(1980) 260

  31. [31]

    A Simple Solution to the Strong CP Problem with a Harmless Axion,

    M. Dine, W. Fischler, and M. Srednicki, “A Simple Solution to the Strong CP Problem with a Harmless Axion,”Phys. Lett. B104(1981) 199–202

  32. [32]

    µ→eγat a Rate of One Out of 10 9 Muon Decays?,

    P. Minkowski, “µ→eγat a Rate of One Out of 10 9 Muon Decays?,”Phys. Lett. B67(1977) 421–428

  33. [33]

    Neutrino Mass and Spontaneous Parity Nonconservation,

    R. N. Mohapatra and G. Senjanovic, “Neutrino Mass and Spontaneous Parity Nonconservation,”Phys. Rev. Lett.44(1980) 912

  34. [34]

    Resonant leptogenesis,

    A. Pilaftsis and T. E. J. Underwood, “Resonant leptogenesis,”Nucl. Phys. B692(2004) 303–345, arXiv:hep-ph/0309342. [39]NA62Collaboration, E. Cortina Gilet al., “Searches for hidden sectors usingK + →π +Xdecays,”JHEP11 (2025) 143,arXiv:2507.17286 [hep-ex]. [40]HIKECollaboration, M. U. Ashrafet al., “High Intensity Kaon Experiments (HIKE) at the CERN SPS Pr...

  35. [35]

    Probing intermediate scale Froggatt-Nielsen models at future gravitational wave observatories,

    D. Ringe, “Probing intermediate scale Froggatt-Nielsen models at future gravitational wave observatories,” Phys. Rev. D107no. 1, (2023) 015030, arXiv:2208.07778 [hep-ph]

  36. [36]

    Gravitational waves from cosmic strings in Froggatt-Nielsen flavour models,

    S. Blasi, L. Calibbi, A. Mariotti, and K. Turbang, “Gravitational waves from cosmic strings in Froggatt-Nielsen flavour models,”JHEP05(2025) 019, arXiv:2410.08668 [hep-ph]

  37. [37]

    Gravity tidings from domain walls: Flavour hierarchies are making waves,

    S. Antusch, I. de Medeiros Varzielas, and M. Levy, “Gravity tidings from domain walls: Flavour hierarchies are making waves,”arXiv:2603.23395 [hep-ph]

  38. [38]

    Axion Mass Prediction from Adaptive Mesh Refinement Cosmological Lattice Simulations,

    J. N. Benabou, M. Buschmann, J. W. Foster, and B. R. Safdi, “Axion Mass Prediction from Adaptive Mesh Refinement Cosmological Lattice Simulations,”Phys. Rev. Lett.134no. 24, (2025) 241003, arXiv:2412.08699 [hep-ph]

  39. [39]

    Spectrum of global string networks and the axion dark matter mass,

    K. Saikawa, J. Redondo, A. Vaquero, and M. Kaltschmidt, “Spectrum of global string networks and the axion dark matter mass,”JCAP10(2024) 043, arXiv:2401.17253 [hep-ph]

  40. [40]

    Planck scale symmetry breaking and majoron physics,

    I. Z. Rothstein, K. S. Babu, and D. Seckel, “Planck scale symmetry breaking and majoron physics,”Nucl. Phys. B403(1993) 725–748,arXiv:hep-ph/9301213

  41. [41]

    Probing the pre-BBN universe with gravitational waves from cosmic strings,

    Y. Cui, M. Lewicki, D. E. Morrissey, and J. D. Wells, “Probing the pre-BBN universe with gravitational waves from cosmic strings,”JHEP01(2019) 081, arXiv:1808.08968 [hep-ph]

  42. [42]

    Gauged global strings,

    X. Niu, W. Xue, and F. Yang, “Gauged global strings,” JHEP02(2024) 093,arXiv:2311.07639 [hep-ph]

  43. [43]

    String Decomposition and Gravitational Waves in High-quality Axion Gauge Theories,

    C. Mupo and Y. Zhang, “String Decomposition and Gravitational Waves in High-quality Axion Gauge Theories,”arXiv:2510.23738 [hep-ph]

  44. [44]

    Gravitational waves from global cosmic strings and cosmic archaeology,

    C.-F. Chang and Y. Cui, “Gravitational waves from global cosmic strings and cosmic archaeology,”JHEP 03(2022) 114,arXiv:2106.09746 [hep-ph]

  45. [45]

    High-quality axion dark matter at gravitational wave interferometers,

    D. Bandyopadhyay, D. Borah, N. Das, and R. Samanta, “High-quality axion dark matter at gravitational wave interferometers,”Phys. Rev. D113no. 9, (2026) 095025,arXiv:2509.14323 [hep-ph]

  46. [46]

    Improved constraint on the primordial gravitational-wave density using recent cosmological data and its impact on cosmic string models,

    S. Henrot-Versilleet al., “Improved constraint on the primordial gravitational-wave density using recent cosmological data and its impact on cosmic string models,”Class. Quant. Grav.32no. 4, (2015) 045003, arXiv:1408.5299 [astro-ph.CO]

  47. [47]

    A Cosmological Bound on the Invisible Axion,

    L. F. Abbott and P. Sikivie, “A Cosmological Bound on the Invisible Axion,”Phys. Lett. B120(1983) 133–136

  48. [48]

    Axionic domain walls at Pulsar Timing Arrays: QCD bias and particle friction,

    S. Blasi, A. Mariotti, A. Rase, and A. Sevrin, “Axionic domain walls at Pulsar Timing Arrays: QCD bias and particle friction,”JHEP11(2023) 169, arXiv:2306.17830 [hep-ph]. [57]PlanckCollaboration, P. A. R. Adeet al., “Planck 2013 results. XVI. Cosmological parameters,”Astron. Astrophys.571(2014) A16,arXiv:1303.5076 [astro-ph.CO]

  49. [49]

    STRETCHING COSMIC STRINGS,

    N. Turok and P. Bhattacharjee, “STRETCHING COSMIC STRINGS,”Phys. Rev. D29(1984) 1557

  50. [50]

    Scaling of cosmic string loops,

    V. Vanchurin, K. D. Olum, and A. Vilenkin, “Scaling of cosmic string loops,”Phys. Rev. D74(2006) 063527, arXiv:gr-qc/0511159

  51. [51]

    Cosmic string loops in the expanding Universe,

    K. D. Olum and V. Vanchurin, “Cosmic string loops in the expanding Universe,”Phys. Rev. D75(2007) 063521,arXiv:astro-ph/0610419

  52. [52]

    Fractal properties and small-scale structure of cosmic string networks,

    C. J. A. P. Martins and E. P. S. Shellard, “Fractal properties and small-scale structure of cosmic string networks,”Phys. Rev. D73(2006) 043515, arXiv:astro-ph/0511792

  53. [53]

    Cosmological evolution of cosmic string loops,

    C. Ringeval, M. Sakellariadou, and F. Bouchet, “Cosmological evolution of cosmic string loops,”JCAP 02(2007) 023,arXiv:astro-ph/0511646

  54. [54]

    Stochastic gravitational wave background from smoothed cosmic string loops,

    J. J. Blanco-Pillado and K. D. Olum, “Stochastic gravitational wave background from smoothed cosmic string loops,”Phys. Rev. D96no. 10, (2017) 104046, arXiv:1709.02693 [astro-ph.CO]

  55. [55]

    Gravitational Wave Signature and the Nature of Neutrino Masses: Majorana, Dirac, or Pseudo-Dirac?,

    S. Jana, S. Manna, and V. P. K, “Gravitational Wave Signature and the Nature of Neutrino Masses: Majorana, Dirac, or Pseudo-Dirac?,”Phys. Lett. B877 (2026) 140476,arXiv:2509.10456 [hep-ph]

  56. [56]

    Gravitational Radiation from Cosmic Strings,

    T. Vachaspati and A. Vilenkin, “Gravitational Radiation from Cosmic Strings,”Phys. Rev. D31 (1985) 3052

  57. [57]

    PTArcade,

    A. Mitridate, D. Wright, R. von Eckardstein, T. Schr¨ oder, J. Nay, K. Olum, K. Schmitz, and T. Trickle, “PTArcade,”arXiv:2306.16377 [hep-ph]