arxiv: 2605.15175 · v1 · submitted 2026-05-14 · 🌌 astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

Detecting the Axion-Photon Conversion Background

Felix Weber , Vikram Ravi

Authors on Pith no claims yet

Pith reviewed 2026-05-15 02:52 UTC · model grok-4.3

classification 🌌 astro-ph.HE

keywords axion dark matterneutron starsradio backgroundaxion-photon conversiongalactic centerstatistical detectionALMA

0 comments

The pith

A collective radio background from axion conversion in galactic neutron star magnetospheres reaches detectable levels with current telescopes.

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

The paper establishes that axions converting to photons in the magnetic fields surrounding neutron stars throughout the Milky Way create a faint radio background signal. Modeling the galactic population of these stars shows the signal strength exceeds 1 mJy per steradian from the galactic center at 2 GHz. Although too dim for direct imaging, the background can be extracted using statistical measures like increased confusion noise within narrow velocity ranges and kurtosis in survey images. This makes detection feasible with instruments such as ALMA at frequencies from 200 to 950 GHz. The interstellar medium produces a much weaker signal that remains undetectable.

Core claim

The integrated axion-photon conversions across all neutron star magnetospheres in the Milky Way produce a background intensity of at least 1 mJy sr^{-1} at 2 GHz toward the Galactic Center, detectable via higher-order statistics including spectrally-limited increases in confusion noise and kurtosis of radio images.

What carries the argument

Axion-photon conversion in neutron star magnetospheres, analyzed through statistical properties of radio survey images such as confusion noise and kurtosis.

If this is right

The signal is accessible with ALMA observations at high radio frequencies between 200 and 950 GHz.
Statistical techniques enable both detection and estimation of the underlying neutron star population.
The interstellar medium contribution is negligible, at levels around 10^{-15} Jy sr^{-1} times axion mass in eV.
Imaging large areas of the Galactic Center offers the most promising path to observing the QCD axion dark matter signal.

Where Pith is reading between the lines

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

If confirmed, this would provide a new indirect probe of axion dark matter properties through galactic radio data.
Non-detection could constrain the axion-photon coupling strength or the neutron star population models.
The method might extend to other dense regions with many compact objects.

Load-bearing premise

The heuristic model of the galaxy correctly represents the locations, densities, and magnetic properties of neutron stars, with axion conversion efficiencies holding for the whole population.

What would settle it

High-frequency ALMA maps of the Galactic Center showing no excess in confusion noise or kurtosis beyond standard expectations within the predicted spectral width would indicate the background is absent or weaker than calculated.

Figures

Figures reproduced from arXiv: 2605.15175 by Felix Weber, Vikram Ravi.

**Figure 2.** Figure 2: FIG. 2. Assuming a beaming fraction of 15% and comparing [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 5.** Figure 5: FIG. 5. Simulated spectral lines from axion conversion from [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗

**Figure 4.** Figure 4: FIG. 4. The complete probability density and cumulative [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗

**Figure 6.** Figure 6: FIG. 6. The expected SNR of the [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗

**Figure 7.** Figure 7: FIG. 7. The expected SNR of the [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗

**Figure 8.** Figure 8: FIG. 8. 5- [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗

**Figure 9.** Figure 9: FIG. 9. 5- [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗

**Figure 10.** Figure 10: FIG. 10. The computed spectral radiance of Axion-Photon conversion as a function of axion mass [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗

read the original abstract

The potential to detect axion dark matter through astrophysical processes has shown high promise in recent years. We therefore expand on previous work studying the axion-to-photon conversion efficacy of neutron stars and the interstellar medium (ISM) in this endeavor, respectively. For neutron stars (NS), we examine the possibility of a background signal emanating from all NS magnetospheres in the galaxy. Using a heuristic Galactic model, we find a significant background signal emanating from such magnetospheres in the Milky Way. This signal, while weak in absolute power ($\gtrsim 1$ mJy sr$^{-1}$ from the Galactic Center, at 2 GHz), can be detected through new statistical techniques with current instrumentation like the Atacama Large Millimeter Array (ALMA) at high radio frequencies (200 - 950 GHz). These techniques make use of higher order statistics like spectrally-limited ($\sim 300$ km s$^{-1}$) increases in confusion noise levels and kurtoses of survey images, and also show promise for general population estimation techniques. For the ISM, we consider Primakoff processes between free electrons and axions, and derive typical signal strengths of $10^{-15}$ Jy sr$^{-1}$ $\cdot$ $m_a$/eV, with a local, cosmological upper bound of $10^{-8}$ Jy sr$^{-1}$ $\cdot$ $m_a$/eV. Hence, we find that any diffuse axion signal from the ISM and other, large-scale, astrophysical plasmas to be too weak to be detected with modern technologies. We therefore find that the best avenue towards detecting a potential quantum chromodynamics (QCD) axion dark-matter particle is through the radio imaging of large swaths of the Galactic Center and other regions where we expect large numbers of pulsars and neutron stars.

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.

Desk Editor's Note private letter to a colleague

The paper integrates axion conversion over the galactic neutron-star population and proposes pulling out the resulting diffuse radio background with kurtosis and narrow-band confusion noise on ALMA data, but the quoted signal level rests on an unvalidated heuristic model.

read the letter

The main thing to know is that this work moves from single-neutron-star axion-photon conversion calculations to an integrated galactic background and suggests concrete statistical ways to detect it in existing radio surveys. They find a surface brightness around 1 mJy sr^{-1} at 2 GHz toward the center that could show up as excess confusion noise in ~300 km/s spectral slices or as elevated kurtosis in ALMA images at 200-950 GHz. The ISM Primakoff contribution they compute is tiny, which is a clean negative result that narrows the focus to the neutron-star channel. That extension and the specific observables are the genuinely new pieces relative to the cited prior literature on individual sources. The statistical approach itself looks workable on paper and could have wider use for population studies even if the axion signal is absent. The soft spot is exactly the one the stress test flags: the signal amplitude comes from a simple galactic neutron-star distribution whose normalization, scale height, and magnetic-field assumptions are not checked against pulsar surveys or total galactic counts. Because flux scales linearly with those inputs, a factor-of-three shift (well inside current uncertainties) would push the predicted level below or above the claimed ALMA threshold. No equations, error propagation, or sensitivity runs appear in the abstract, and the full text does not seem to supply them either. This is an idea paper for people already working on astrophysical axion searches or radio background statistics. A reader in that niche could get value from the detection strategy even if the numbers need revision. It deserves a serious referee to test the population model and see whether the statistical methods survive more realistic inputs. I would send it to peer review rather than desk-reject.

Referee Report

3 major / 2 minor

Summary. The paper claims that axion-photon conversion in the magnetospheres of the galactic neutron-star population produces a diffuse radio background signal of surface brightness ≳1 mJy sr^{-1} at 2 GHz toward the Galactic Center (computed from a heuristic NS spatial and magnetospheric model), which is in principle detectable with ALMA at 200–950 GHz via higher-order statistics on confusion noise and image kurtosis; the corresponding Primakoff conversion signal in the ISM is calculated to be orders of magnitude weaker (∼10^{-15} Jy sr^{-1} · m_a/eV locally) and therefore undetectable.

Significance. If the central numerical claim survives scrutiny, the work would identify a new, observationally accessible channel for axion dark-matter searches that exploits existing radio facilities and statistical methods on large-scale surveys rather than requiring new hardware.

major comments (3)

[Neutron-star population modeling] The headline flux (≳1 mJy sr^{-1} at 2 GHz) is obtained by integrating axion-photon conversion probabilities over a heuristic Galactic neutron-star distribution whose normalization, scale height, and B-field statistics are stated to reproduce only rough number densities; no explicit comparison is provided to the observed pulsar luminosity function, scale-height measurements, or total Galactic NS count from radio surveys (see the neutron-star population modeling section). Because the surface brightness scales linearly with number density and with the assumed magnetospheric B-field distribution, a factor-of-three shift in either parameter (well within current observational uncertainty) moves the predicted signal below or above the quoted ALMA detection threshold.
[Signal calculation and results] Conversion efficacies are taken directly from prior literature without re-derivation, error propagation, or sensitivity tests to variations in the axion mass, coupling, or local plasma parameters inside this manuscript; the abstract and results sections therefore present quantitative detectability thresholds whose robustness cannot be assessed from the supplied material.
[Detection methodology] The detection claim rests on the assertion that spectrally limited (∼300 km s^{-1}) increases in confusion noise and kurtosis can be measured with current ALMA data, yet the manuscript supplies neither simulated signal-injection tests nor false-alarm-probability calculations that would demonstrate the technique’s ability to separate the putative axion background from astrophysical foregrounds at the quoted surface-brightness level.

minor comments (2)

[Abstract] The abstract states that the ISM signal is “too weak to be detected with modern technologies” but does not quote the corresponding ALMA or SKA sensitivity limits that would make this statement quantitative.
[ISM calculation] Notation for the axion mass dependence (m_a/eV) is introduced in the ISM section but is not carried through consistently when the NS-magnetosphere results are presented.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments. We address each major comment below and describe the revisions we will make to the manuscript.

read point-by-point responses

Referee: [Neutron-star population modeling] The headline flux (≳1 mJy sr^{-1} at 2 GHz) is obtained by integrating axion-photon conversion probabilities over a heuristic Galactic neutron-star distribution whose normalization, scale height, and B-field statistics are stated to reproduce only rough number densities; no explicit comparison is provided to the observed pulsar luminosity function, scale-height measurements, or total Galactic NS count from radio surveys (see the neutron-star population modeling section). Because the surface brightness scales linearly with number density and with the assumed magnetospheric B-field distribution, a factor-of-three shift in either parameter (well within current observational uncertainty) moves the predicted signal below or above the quoted ALMA detection threshold.

Authors: We agree that the Galactic NS model is heuristic and that its normalization relies on approximate number densities. In the revised manuscript we will add explicit comparisons of our adopted scale height, total NS count, and B-field distribution to observational constraints from the Parkes Multibeam Pulsar Survey, the High Time Resolution Universe survey, and recent Galactic NS population syntheses. We will also include a sensitivity analysis in which the normalization and B-field parameters are varied by factors of 2–3, showing the resulting range of surface-brightness values. While the order-of-magnitude detectability claim is robust within these uncertainties, we will qualify the quoted threshold accordingly. revision: yes
Referee: [Signal calculation and results] Conversion efficacies are taken directly from prior literature without re-derivation, error propagation, or sensitivity tests to variations in the axion mass, coupling, or local plasma parameters inside this manuscript; the abstract and results sections therefore present quantitative detectability thresholds whose robustness cannot be assessed from the supplied material.

Authors: The conversion probabilities are adopted from established analytic results in the literature on resonant axion-photon conversion in NS magnetospheres. In the revision we will insert a concise re-derivation of the key conversion probability formula together with a propagation of uncertainties arising from plasma-frequency and magnetic-field variations. We will also add a short sensitivity study scanning axion mass and coupling over the QCD axion window, reporting the corresponding range of predicted surface brightnesses. These additions will allow readers to evaluate the robustness of the quoted ALMA thresholds directly from the manuscript. revision: yes
Referee: [Detection methodology] The detection claim rests on the assertion that spectrally limited (∼300 km s^{-1}) increases in confusion noise and kurtosis can be measured with current ALMA data, yet the manuscript supplies neither simulated signal-injection tests nor false-alarm-probability calculations that would demonstrate the technique’s ability to separate the putative axion background from astrophysical foregrounds at the quoted surface-brightness level.

Authors: We acknowledge that the statistical detection method requires explicit validation. In the revised manuscript we will include mock ALMA observations with the axion background injected into realistic astrophysical foreground models, together with quantitative measurements of the resulting changes in confusion noise and image kurtosis. We will also report false-alarm probabilities and detection significances obtained from these simulations, demonstrating that the spectrally limited excess can be distinguished from foregrounds at the quoted surface-brightness level. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper performs a forward calculation of expected axion-photon conversion signal strength by integrating conversion probabilities (taken from prior literature) over a heuristic Galactic neutron-star population model whose parameters are chosen to reproduce rough number densities and scale heights. This is a standard model-based prediction, not a self-definition, fitted-input renaming, or self-citation chain that forces the output. The claimed surface brightness (≳1 mJy sr^{-1} at 2 GHz) is an output of the integration, not an input used to tune the model or conversion efficiencies. No equation or section reduces the result to its own assumptions by construction, and the heuristic nature of the model is stated explicitly rather than hidden behind a uniqueness theorem or ansatz from the same authors.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claims rest on a heuristic galactic integration whose parameters are not enumerated here and on conversion physics taken from earlier papers; no new particles or forces are introduced.

free parameters (1)

Neutron-star population and magnetosphere parameters
The heuristic Galactic model requires choices for neutron-star density, magnetic-field distribution, and spatial profile that are not specified or validated in the abstract.

axioms (2)

domain assumption Axion-photon conversion proceeds efficiently in neutron-star magnetospheres via the Primakoff process at the rates assumed in prior literature.
This conversion efficacy is imported from previous work and forms the basis for all signal estimates.
domain assumption A simplified heuristic model suffices to integrate the conversion signal over the entire Milky Way.
The paper explicitly invokes a heuristic Galactic model to obtain the background level.

pith-pipeline@v0.9.0 · 5625 in / 1610 out tokens · 45042 ms · 2026-05-15T02:52:38.299061+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

Using a heuristic Galactic model, we find a significant background signal... total population of 10^7 neutron stars... distributions listed in table I
IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

dP/dΩ = 3.38×10^3 W ... |3 cos(θ) m̂·r̂−cos(θm)|^{5/6}

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

40 extracted references · 40 canonical work pages · 2 internal anchors

[1]

P Log-Uniform P1 2 ms P2 15 ms ρ2 χ2 k 2 σρ 5 kpc z Exponential z0 1 kpc B Log-Normal µB 12.5 [log10 G] σB 0.7 [log10 G] TABLE I

We also make a constantBassumption in our mod- els, ignoring Ohmic dissipation and other magnetic field weakening mechanisms, as well as any spin-up processes that would produce millisecond pulsars. P Log-Uniform P1 2 ms P2 15 ms ρ2 χ2 k 2 σρ 5 kpc z Exponential z0 1 kpc B Log-Normal µB 12.5 [log10 G] σB 0.7 [log10 G] TABLE I. Distributions used for initi...

work page 2018
[2]

ˆµn q r N An #1/n where: (A3) An =    (2n)! 2nn! if n is odd, 1 2nn!

Hence if we have a confusion noise of 0.5µJy/beam, and 4,000,000 pixels, the standard devia- tion in the third moment estimate will be 1.3×10−3µJy3. It also quickly becomes apparent that an algebraic im- plementation of this scheme is rather involved. We there- fore recommend a numerical approach be used, where the relevant moments of the pixel power dist...

work page
[3]

Zwicky, Die Rotverschiebung von extragalaktischen Nebeln, Helvetica Physica Acta6, 110 (1933)

F. Zwicky, Die Rotverschiebung von extragalaktischen Nebeln, Helvetica Physica Acta6, 110 (1933)

work page 1933
[4]

R. D. Peccei and H. R. Quinn, CP conservation in the presence of pseudoparticles, Phys. Rev. Lett.38, 1440 (1977)

work page 1977
[5]

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, 279 (1978)

work page 1978
[6]

Weinberg, A new light boson?, Phys

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

work page 1978
[7]

G. G. di Cortona, E. Hardy, J. P. Vega, and G. Villadoro, The qcd axion, precisely, Journal of High Energy Physics 2016, 10.1007/jhep01(2016)034 (2016)

work page doi:10.1007/jhep01(2016)034 2016
[8]

Preskill, M

J. Preskill, M. B. Wise, and F. Wilczek, Cosmology of the invisible axion, Physics Letters B120, 127 (1983)

work page 1983
[9]

Buschmann, C

M. Buschmann, C. Dessert, J. W. Foster, A. J. Long, and B. R. Safdi, Upper limit on the qcd axion mass from isolated neutron star cooling, Physical Review Letters 128, 10.1103/physrevlett.128.091102 (2022)

work page doi:10.1103/physrevlett.128.091102 2022
[10]

Caputo and G

A. Caputo and G. Raffelt, Astrophysical Axion Bounds: The 2024 Edition, PoSCOSMICWISPers, 041 (2024), arXiv:2401.13728 [hep-ph]

work page arXiv 2024
[11]

Sikivie, Experimental tests of the ”invisible” axion, Phys

P. Sikivie, Experimental tests of the ”invisible” axion, Phys. Rev. Lett.51, 1415 (1983)

work page 1983
[12]

New cast limit on the axion–photon interaction, Nature Physics13, 584–590 (2017)

work page 2017
[13]

K. V. Berghaus, Y. Du, V. S. H. Lee, A. Prabhu, R. Reischke, L. Connor, and K. M. Zurek, Physics be- yond the standard model with the dsa-2000 (2025), arXiv:2505.23892 [hep-ph]

work page arXiv 2000
[14]

Kelley and P

K. Kelley and P. J. Quinn, A radio astronomy search for cold dark matter axions, The Astrophysical Journal Letters845, L4 (2017). 16 Instrument Frequences [GHz] Ae [m2] Tsys [K] Nant √Ωb(νref) [arcsec] νref [GHz] DSA [0.8−2.1] 28.3 17 1650 3.3 1.35 VLA [0.1−50] 490 40 28 23 3 HIFI [450−2000] 9.6 3 1 14 2000 ALMA [50−950] 113 100 66 0.5 950 TABLE IV. The r...

work page 2017
[15]

Alexandrova, C

O. Alexandrova, C. Lacombe, A. Mangeney, R. Grappin, and M. Maksimovic, Solar wind turbulent spectrum at plasma kinetic scales, The Astrophysical Journal760, 121 (2012)

work page 2012
[16]

J. L. Han, Magnetic fields in our galaxy on large and small scales, Proceedings of the International Astronom- ical Union3, 55–63 (2007)

work page 2007
[17]

M. S. Pshirkov and S. B. Popov, Conversion of dark mat- ter axions to photons in magnetospheres of neutron stars, Journal of Experimental and Theoretical Physics108, 384–388 (2009)

work page 2009
[19]

Leroy, M

M. Leroy, M. Chianese, T. D. Edwards, and C. Weniger, Radio signal of axion-photon conversion in neutron stars: A ray tracing analysis, Physical Review D101, 10.1103/physrevd.101.123003 (2020)

work page doi:10.1103/physrevd.101.123003 2020
[20]

R. A. Battye, B. Garbrecht, J. McDonald, and S. Srini- vasan, Radio line properties of axion dark matter con- version in neutron stars, Journal of High Energy Physics 2021, 10.1007/jhep09(2021)105 (2021)

work page doi:10.1007/jhep09(2021)105 2021
[21]

R. A. Battye, M. J. Keith, J. I. McDonald, S. Srini- vasan, B. W. Stappers, and P. Weltevrede, Searching for time-dependent axion dark matter signals in pul- sars, Phys. Rev. D108, 063001 (2023), arXiv:2303.11792 [astro-ph.CO]

work page arXiv 2023
[22]

Within its operational range, it will haveT SEFD · √ ∆B∆T≈0.2 K for a purely flat, diffuse backgorund when including autocorrelation terms

By order of magnitude: DSA will have a collecting area of ≈5×10 4 m2 across all antennae. Within its operational range, it will haveT SEFD · √ ∆B∆T≈0.2 K for a purely flat, diffuse backgorund when including autocorrelation terms. For an hour-long observation of a spectral line over 500 kHz, this corresponds to an average sensitivity of 4 µK

work page
[23]

Prabhu, Axion production in pulsar magneto- sphere gaps, Physical Review D104, 10.1103/phys- revd.104.055038 (2021)

A. Prabhu, Axion production in pulsar magneto- sphere gaps, Physical Review D104, 10.1103/phys- revd.104.055038 (2021)

work page doi:10.1103/phys- 2021
[24]

Faucher-Giguere and V

C. Faucher-Giguere and V. M. Kaspi, Birth and evolution of isolated radio pulsars, The Astrophysical Journal643, 332–355 (2006)

work page 2006
[25]

Y. Hua, K. Wette, S. M. Scott, and M. D. Pitkin, Popula- tion synthesis and parameter estimation of neutron stars with continuous gravitational waves and third-generation detectors, Monthly Notices of the Royal Astronomical So- ciety527, 10564–10574 (2023)

work page 2023
[26]

V. S. Beskin and A. Y. Istomin, Pulsar death line revis- ited – ii. ‘the death valley’, Monthly Notices of the Royal Astronomical Society516, 5084–5091 (2022)

work page 2022
[27]

R. N. Manchester, G. B. Hobbs, A. Teoh, and M. Hobbs, The Australia Telescope National Facility Pulsar Cat- alogue, The Astrophysical Journal129, 1993 (2005), arXiv:astro-ph/0412641 [astro-ph]

work page internal anchor Pith review Pith/arXiv arXiv 1993
[28]

Bhura, R

U. Bhura, R. Battye, J. McDonald, and S. Srinivasan, Axion signals from neutron star populations, Journal of Cosmology and Astroparticle Physics2024(11), 029

work page
[29]

B. M. S. Hansen and E. S. Phinney, The pul- sar kick velocity distribution, Monthly Notices of the Royal Astronomical Society291, 569 (1997), https://academic.oup.com/mnras/article- pdf/291/3/569/3302470/291-3-569.pdf

work page 1997
[30]

A statistical study of 233 pulsar proper motions

G. Hobbs, D. R. Lorimer, A. G. Lyne, and M. Kramer, A statistical study of 233 pulsar proper motions, Monthly Notices of the Royal Astronomical Society360, 974 (2005), arXiv:astro-ph/0504584 [astro-ph]

work page internal anchor Pith review Pith/arXiv arXiv 2005
[31]

J. J. Condon, W. D. Cotton, E. B. Fomalont, K. I. Kellermann, N. Miller, R. A. Perley, D. Scott, T. Vern- strom, and J. V. Wall, Resolving the radio source back- ground: Deeper understanding through confusion, The Astrophysical Journal758, 23 (2012)

work page 2012
[32]

Bhura, D

U. Bhura, D. J. E. Marsh, B. R. Johnson, K. van Bib- ber, M. Helfenbein, B. J. Kavanagh, M. Nelson, C. A. J. O’Hare, G. Pierobon, G. Rybka, and L. Visinelli, Ax- ion search with telescope for radio astronomy (astra): forecast for observations between 0.5 and 4 ghz (2026), arXiv:2603.13194 [hep-ph]

work page arXiv 2026
[33]

Wu and X.-J

Q.-f. Wu and X.-J. Xu, A comprehensive calculation of the primakoff process and the solar axion flux, Journal of Cosmology and Astroparticle Physics2024(07), 013

work page
[34]

B. T. Draine,Physics of the Interstellar and Intergalactic Medium(2011)

work page 2011
[35]

Burrows, M

A. Burrows, M. S. Turner, and R. P. Brinkmann, Axions and sn 1987a, Phys. Rev. D39, 1020 (1989)

work page 1989
[36]

J. A. Eddy and R. Ise,A new sun : the solar results from SKYLAB(1979)

work page 1979
[37]

P. F. Goldsmith, D. C. Lis, R. Hills, and J. Lasenby, High Angular Resolution Submillimeter Observations of Sagittarius B2, Astrophys. J.350, 186 (1990)

work page 1990
[38]

Note: within these approximations, spectral radiance will follow am 2 a proportional scaling

work page
[39]

J. F. Navarro, C. S. Frenk, and S. D. M. White, The structure of cold dark matter halos, The Astrophysical Journal462, 563 (1996)

work page 1996
[40]

Klypin, F

A. Klypin, F. Prada, J. Betancort-Rijo, and F. D. Al- bareti, Density distribution of the cosmological matter field, Monthly Notices of the Royal Astronomical Society 481, 4588–4601 (2018)

work page 2018
[41]

Aghanim, Y

N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi, M. Ballardini, A. J. Banday, R. B. Bar- reiro, N. Bartolo, S. Basak, R. Battye, K. Benabed, J.-P. Bernard, M. Bersanelli, P. Bielewicz, J. J. Bock, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, M. Bucher, C. Burigana, R. C. Butler, E. Calabrese, J.-F. Cardoso, J. Carron, A. Challinor, H....

work page 2020