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arxiv: 2604.16154 · v2 · submitted 2026-04-17 · 🌌 astro-ph.CO · gr-qc· hep-th

Recognition: unknown

Probing Primordial Black Holes with upcoming Radio Telescopes: a case study for LOFAR2.0, FAST Core Array and BINGO

Amilcar R. Queiroz, Guillem Dom\`enech, Joao R. L. Santos

Pith reviewed 2026-05-10 07:31 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-th
keywords primordial black holesfast radio burstsgravitational lensingdark matterradio telescopescosmologyLOFARBINGO
0
0 comments X

The pith

Upcoming radio telescopes can bound the fraction of dark matter in primordial black holes using lensed fast radio bursts.

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

The paper shows that searches for lensed fast radio bursts with upcoming telescopes offer a way to test if primordial black holes make up a significant part of dark matter. It forecasts that LOFAR2.0 could limit this fraction to below 0.16 for black holes more massive than the Sun. FAST Core Array and BINGO could set a limit of 0.39 for somewhat different mass ranges. This matters because it adds an independent check using radio observations that will grow stronger with more data on bursts. If true, it helps narrow down whether early-universe black holes can solve the dark matter problem without conflicting with other observations.

Core claim

The central claim is that the absence of observed lensed FRB events in surveys by LOFAR2.0, FAST Core Array, and BINGO will translate into upper limits on the PBH dark matter fraction f_PBH of 0.16 for M_PBH > 1 M_sun with LOFAR2.0, and 0.39 for M_PBH > 10 M_sun with FAST and M_PBH > 10^{-2} M_sun with BINGO, based on calculated lensing probabilities and expected event rates.

What carries the argument

The lensing optical depth for FRBs due to PBHs, which determines the probability of detecting multiply-imaged bursts and depends on the PBH mass and their fraction of dark matter.

If this is right

  • Non-observation of lensed FRBs with LOFAR2.0 implies f_PBH < 0.16 for masses above 1 solar mass.
  • FAST Core Array can restrict f_PBH < 0.39 for PBHs heavier than 10 solar masses.
  • BINGO provides a bound f_PBH < 0.39 for PBHs above 0.01 solar masses.
  • FRB lensing acts as an independent and complementary test of the PBH scenario.
  • Larger future catalogs of FRBs will strengthen these constraints over time.

Where Pith is reading between the lines

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

  • Higher than assumed FRB rates would allow even tighter bounds on PBH abundance from the same telescopes.
  • This radio lensing approach could be extended to other upcoming surveys to cover more PBH mass ranges.
  • If PBHs are ruled out in these windows, attention may shift to other dark matter candidates like axions or WIMPs.

Load-bearing premise

The calculations depend on particular assumptions about the overall rate and redshift distribution of FRBs as well as the precise lensing optical depth.

What would settle it

Finding a number of lensed FRB events much larger than the background expectation in the LOFAR2.0 survey would indicate either a higher PBH fraction or that the FRB assumptions need revision.

Figures

Figures reproduced from arXiv: 2604.16154 by Amilcar R. Queiroz, Guillem Dom\`enech, Joao R. L. Santos.

Figure 1
Figure 1. Figure 1: FIG. 1: Lens plane to characterize the detectability of ∆ [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Histogram of the recent data of 131 confirmed FRB events. The fit (2.16) is shown with [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Total optical depth for LOFAR, FAST, and BINGO. In these graphics, we consider the [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Forecast for the fraction of primordial black holes allowed as point lenses. [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: Constraints on the fraction of primordial black holes from different surveys combined [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
read the original abstract

Fast Radio Bursts (FRBs) are among the most intriguing phenomena observed in radio astronomy. So far, about 130 FRB signals have been confirmed and characterized by different surveys, and the CHIME telescope has recently reported a new catalog of 4539 bursts. Therefore, these numbers are expected to increase in the coming years. The detection, or lack thereof, of lensed FRB events can be used to probe Primordial Black Holes (PBHs) as a fraction of dark matter. We investigate the potential of three upcoming radio telescopes, LOFAR2.0, FAST Core Array, and BINGO, to test the PBH scenario. We forecast that LOFAR2.0 will constrain $f_{\mathrm{PBH}} < 0.16$ for PBH masses $M_{\rm PBH}>1\,{M_{\odot}}$, while FAST Core Array and BINGO will restrict $f_{\mathrm{PBH}} < 0.39$ for $M_{\rm PBH}>10\,{M_{\odot}}$ and $M_{\rm PBH}>10^{-2}\,{M_{\odot}}$, respectively. Despite the existence of stricter constraints, FRB lensing offers an independent and complementary probe of PBHs in the Universe, which will improve in the future.

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

1 major / 2 minor

Summary. The manuscript forecasts upper limits on the primordial black hole dark matter fraction f_PBH using the non-detection of gravitationally lensed fast radio bursts (FRBs) observable by three upcoming radio telescopes. It claims LOFAR2.0 can reach f_PBH < 0.16 for M_PBH > 1 M_⊙, while FAST Core Array and BINGO reach f_PBH < 0.39 for M_PBH > 10 M_⊙ and M_PBH > 10^{-2} M_⊙ respectively. The forecasts combine assumed FRB detection rates and redshift distributions with standard PBH point-mass lensing optical depths and telescope-specific detection efficiencies.

Significance. If the underlying FRB population models and lensing calculations hold, the work supplies an independent radio-based probe of PBHs in the stellar-mass range that is complementary to existing microlensing and gravitational-wave bounds. The paper correctly notes that stricter limits already exist but emphasizes the method's future improvement with larger FRB samples. The significance is reduced by the absence of robustness tests against plausible variations in the input FRB models.

major comments (1)
  1. [Abstract and §3] Abstract and forecasting methodology: the headline limits are obtained by setting the expected number of detectable lensed FRBs equal to a small threshold (~1-3 events). This expectation is proportional to the integral over dN_FRB/dz × τ_lens(f_PBH, M_PBH, z) × f_det(z). No alternative FRB redshift distributions, luminosity functions, or evolution scenarios are explored; a factor-of-two shift in the high-z tail directly rescales the quoted f_PBH bounds by the same factor, making the numerical claims load-bearing on untested model choices.
minor comments (2)
  1. [Abstract] The abstract states that 'about 130 FRB signals have been confirmed' while citing the CHIME catalog of 4539 bursts; a brief clarification of the distinction between confirmed and total detected events would improve clarity.
  2. No table or figure shows the sensitivity curves or the explicit dependence of the expected event rate on telescope parameters; adding one would make the forecasts more transparent.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful reading and constructive feedback. We address the single major comment below and will incorporate revisions to strengthen the presentation of our forecasting methodology.

read point-by-point responses

  1. Referee: [Abstract and §3] Abstract and forecasting methodology: the headline limits are obtained by setting the expected number of detectable lensed FRBs equal to a small threshold (~1-3 events). This expectation is proportional to the integral over dN_FRB/dz × τ_lens(f_PBH, M_PBH, z) × f_det(z). No alternative FRB redshift distributions, luminosity functions, or evolution scenarios are explored; a factor-of-two shift in the high-z tail directly rescales the quoted f_PBH bounds by the same factor, making the numerical claims load-bearing on untested model choices.

    Authors: We agree that the quoted limits depend on the adopted FRB population model. In §3 we use a fiducial redshift distribution and detection-rate normalization drawn from the CHIME catalog and other current surveys, which is the standard approach for such forecasts. We did not perform a full parameter scan over alternative luminosity functions or evolution scenarios. In the revised manuscript we will add a short subsection (or paragraph in §3) that explicitly states the linear scaling of the expected lensed-event rate with the high-z tail and illustrates how a factor-of-two change in that tail would rescale the f_PBH bounds. This addition will make the model dependence transparent without altering the headline numbers derived from the fiducial model. revision: partial

Circularity Check

0 steps flagged

No circularity in the forecast derivation for PBH constraints

full rationale

The paper computes expected numbers of lensed FRBs for LOFAR2.0, FAST Core Array and BINGO by integrating an external FRB redshift distribution (extrapolated from CHIME) times the standard PBH point-mass lensing optical depth (linear in f_PBH) times a detection efficiency factor. Upper limits on f_PBH are obtained by requiring this expectation to fall below a small integer threshold. This is a forward calculation from stated model inputs and telescope parameters; no equation, fit, or self-citation reduces the quoted bounds (f_PBH < 0.16 etc.) back to the inputs by construction. The derivation contains no self-definitional steps, fitted-input predictions, load-bearing self-citations, or imported uniqueness theorems.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review supplies no explicit list of free parameters or axioms; typical hidden inputs include assumed all-sky FRB rate, redshift evolution, and PBH mass function shape.

pith-pipeline@v0.9.0 · 5572 in / 1111 out tokens · 37952 ms · 2026-05-10T07:31:37.496413+00:00 · methodology

discussion (0)

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Constraints on the baryon density from fast radio bursts using a non-parametric reconstruction of the Hubble parameter

    astro-ph.CO 2026-05 conditional novelty 5.0

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Reference graph

Works this paper leans on

140 extracted references · 123 canonical work pages · cited by 1 Pith paper · 2 internal anchors

  1. [1]

    We find that a fit toN(z) in the histogram of Fig

    to constrain Hubble and cosmographic parameters. We find that a fit toN(z) in the histogram of Fig. 2 is given by a Gamma distribution, whose explicit form is N(z) =N 0 za1 e−a2 z ;N 0 = 208.7210 ;a 1 = 0.2465 ;a 2 = 4.6269.(2.16) To reach this fit, we tested three different distributions: the Lognormal, Gamma, and Weibull. The tests consisted of computin...

    2012

  2. [2]

    4, we present the exclusion regions forf PBH max for each radio telescope

    In the shaded regions of Fig. 4, we present the exclusion regions forf PBH max for each radio telescope. The shaded colored regions unveil the lowest best interval of time resolution of LOFAR (orange), FAST (green), and BINGO (blue), to computef PBH. The shaded gray regions mark the constraints use the highest best interval of time resolution of Tab. I, a...

    2021

  3. [3]

    D. R. Lorimer, M. Bailes, M. A. McLaughlin, D. J. Narkevic, and F. Crawford, Science318, 777 (2007), arXiv:0709.4301 [astro-ph]

    work page arXiv 2007

  4. [4]

    Generalized Distributions of Host Dispersion Measures in the Fast Radio Burst Cosmology

    J.-Y. Jia, D.-C. Qiang, L.-Y. Li, and H. Wei, Generalized distributions of host dispersion measures in the fast radio burst cosmology (2025), arXiv:2510.09463 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  5. [5]

    Abbottet al.(The CHIME/FRB), Astrophys

    T. Abbott et al. (The CHIME/FRB), Astrophys. J. Suppl.283, 34 (2026), arXiv:2601.09399 [astro- ph.HE]

    work page arXiv 2026

  6. [6]

    A. P. Curtin et al., Astrophys. J.972, 125 (2024), arXiv:2404.09242 [astro-ph.HE]

    work page arXiv 2024

  7. [7]

    A. P. Curtin et al., Astrophys. J.992, 206 (2025), arXiv:2411.02870 [astro-ph.HE]

    work page arXiv 2025

  8. [8]

    J. M. Cordes and I. Wasserman, Mon. Not. Roy. Astron. Soc.457, 232 (2016), arXiv:1501.00753 [astro-ph.HE]

    work page arXiv 2016

  9. [9]

    S. B. Popov and K. A. Postnov, (2007), arXiv:0710.2006 [astro-ph]. 14

    work page arXiv 2007

  10. [10]

    Pen and L

    U.-L. Pen and L. Connor, Astrophys. J.807, 179 (2015), arXiv:1501.01341 [astro-ph.HE]

    work page arXiv 2015

  11. [11]

    M. A. Abramowicz, M. Bejger, and M. Wielgus, Astrophys. J.868, 17 (2018), arXiv:1704.05931 [astro-ph.HE]

    work page arXiv 2018

  12. [12]

    G. M. Fuller, A. Kusenko, and V. Takhistov, Phys. Rev. Lett.119, 061101 (2017), arXiv:1704.01129 [astro-ph.HE]

    work page arXiv 2017

  13. [13]

    Kainulainen, S

    K. Kainulainen, S. Nurmi, E. D. Schiappacasse, and T. T. Yanagida, Phys. Rev. D104, 123033 (2021), arXiv:2108.08717 [astro-ph.HE]

    work page arXiv 2021

  14. [14]

    D. W. P. Amaral and E. D. Schiappacasse, Phys. Rev. D110, 083532 (2024), arXiv:2312.09285 [hep- ph]

    work page arXiv 2024

  15. [15]

    B. Carr, S. Clesse, J. Garcia-Bellido, M. Hawkins, and F. Kuhnel, Phys. Rept.1054, 1 (2024), arXiv:2306.03903 [astro-ph.CO]

    work page arXiv 2024

  16. [16]

    C.-M. Deng, Y. Cai, X.-F. Wu, and E.-W. Liang, Phys. Rev. D98, 123016 (2018), arXiv:1812.00113 [astro-ph.HE]

    work page arXiv 2018

  17. [17]

    Meng, Q.-J

    M. Meng, Q.-J. Huang, and C.-M. Deng, Res. Astron. Astrophys.24, 095006 (2024)

    2024

  18. [18]

    Kalita, S

    S. Kalita, S. Bhatporia, and A. Weltman, Phys. Dark Univ.48, 101926 (2025), arXiv:2410.01974 [astro-ph.CO]

    work page arXiv 2025

  19. [19]

    J. B. Mu˜ noz and A. Loeb, Phys. Rev. D98, 103518 (2018), arXiv:1809.04074 [astro-ph.CO]

    work page arXiv 2018

  20. [20]

    Walters, Y.-Z

    A. Walters, Y.-Z. Ma, J. Sievers, and A. Weltman, Phys. Rev. D100, 103519 (2019), arXiv:1909.02821 [astro-ph.CO]

    work page arXiv 2019

  21. [21]

    Qiang and H

    D.-C. Qiang and H. Wei, JCAP04, 023, arXiv:2002.10189 [astro-ph.CO]

    work page arXiv 2002

  22. [22]

    J. B. Mu˜ noz, E. D. Kovetz, L. Dai, and M. Kamionkowski, Physical Review Letters117, 10.1103/phys- revlett.117.091301 (2016)

    work page doi:10.1103/phys- 2016

  23. [23]

    T. D. Brandt, Astrophys. J. Lett.824, L31 (2016), arXiv:1605.03665 [astro-ph.GA]

    work page Pith review arXiv 2016

  24. [24]

    Y. K. Wang and F. Y. Wang, Astron. Astrophys.614, A50 (2018), arXiv:1801.07360 [astro-ph.CO]

    work page arXiv 2018

  25. [25]

    H. Xiao, L. Dai, and M. McQuinn, Phys. Rev. D106, 103033 (2022), arXiv:2206.13534 [astro-ph.CO]

    work page arXiv 2022

  26. [26]

    Leunget al., Constraining primordial black holes using fast radio burst gravitational-lens interferometry with CHIME/FRB, Phys

    C. Leung et al., Phys. Rev. D106, 043017 (2022), arXiv:2204.06001 [astro-ph.HE]

    work page arXiv 2022

  27. [27]

    Kalita, S

    S. Kalita, S. Bhatporia, and A. Weltman, JCAP11, 059, arXiv:2308.16604 [gr-qc]

    work page arXiv

  28. [28]

    Profumo, JCAP10, 075, arXiv:2508.06688 [astro-ph.HE]

    S. Profumo, JCAP10, 075, arXiv:2508.06688 [astro-ph.HE]

    work page arXiv

  29. [29]

    Li, S.-J

    J.-H. Li, S.-J. Wang, X.-Y. Zhao, and N. Li, Universe11, 311 (2025)

    2025

  30. [30]

    Y. B. Zel’dovich and I. D. Novikov, Sov. Astron.10, 602 (1967)

    1967

  31. [31]

    Hawking, Mon

    S. Hawking, Mon. Not. Roy. Astron. Soc.152, 75 (1971)

    1971

  32. [32]

    B. J. Carr and S. W. Hawking, Mon. Not. Roy. Astron. Soc.168, 399 (1974)

    1974

  33. [33]

    Carr and F

    B. Carr and F. Kuhnel, Ann. Rev. Nucl. Part. Sci.70, 355 (2020), arXiv:2006.02838 [astro-ph.CO]

    work page arXiv 2020

  34. [34]

    M. Y. Khlopov, Res. Astron. Astrophys.10, 495 (2010), arXiv:0801.0116 [astro-ph]

    work page arXiv 2010

  35. [35]

    K. M. Belotsky, A. D. Dmitriev, E. A. Esipova, V. A. Gani, A. V. Grobov, M. Y. Khlopov, A. A. Kirillov, S. G. Rubin, and I. V. Svadkovsky, Mod. Phys. Lett. A29, 1440005 (2014), arXiv:1410.0203 [astro-ph.CO]

    work page arXiv 2014

  36. [36]

    Mroz et al., Nature548, 183 (2017), arXiv:1707.07634 [astro-ph.EP]

    P. Mroz et al., Nature548, 183 (2017), arXiv:1707.07634 [astro-ph.EP]

    work page arXiv 2017

  37. [37]

    Niikura, M

    H. Niikura, M. Takada, S. Yokoyama, T. Sumi, and S. Masaki, Phys. Rev. D99, 083503 (2019), arXiv:1901.07120 [astro-ph.CO]

    work page arXiv 2019

  38. [38]

    Sugiyama, M

    S. Sugiyama, M. Takada, N. Yasuda, and N. Tominaga, (2026), arXiv:2602.05840 [astro-ph.CO]

    work page arXiv 2026

  39. [39]

    H¨ utsi, M

    G. H¨ utsi, M. Raidal, V. Vaskonen, and H. Veerm¨ ae, JCAP03, 068, arXiv:2012.02786 [astro-ph.CO]

    work page arXiv 2012

  40. [40]

    Inferring black hole formation channels in GWTC-4.0 via parametric mass-spin correlations de- rived from first principles,

    E. Berti, F. Crescimbeni, G. Franciolini, S. Mastrogiovanni, P. Pani, and G. Pierra, Phys. Rev. D113, 043048 (2026), arXiv:2512.03152 [gr-qc]

    work page arXiv 2026

  41. [41]

    K. M. Belotsky, V. I. Dokuchaev, Y. N. Eroshenko, E. A. Esipova, M. Y. Khlopov, L. A. Khromykh, A. A. Kirillov, V. V. Nikulin, S. G. Rubin, and I. V. Svadkovsky, Eur. Phys. J. C79, 246 (2019), arXiv:1807.06590 [astro-ph.CO]

    work page arXiv 2019

  42. [42]

    Kawasaki, A

    M. Kawasaki, A. Kusenko, and T. T. Yanagida, Phys. Lett. B711, 1 (2012), arXiv:1202.3848 [astro- ph.CO]. 15

    work page arXiv 2012

  43. [43]

    J. L. Bernal, A. Raccanelli, L. Verde, and J. Silk, JCAP05, 017, [Erratum: JCAP 01, E01 (2020)], arXiv:1712.01311 [astro-ph.CO]

    work page arXiv 2020

  44. [44]

    C. T. Byrnes, J. Lesgourgues, and D. Sharma, JCAP09, 012, arXiv:2404.18475 [astro-ph.CO]

    work page arXiv

  45. [45]

    Primordial Black Holes - Perspectives in Gravitational Wave Astronomy -

    M. Sasaki, T. Suyama, T. Tanaka, and S. Yokoyama, Class. Quant. Grav.35, 063001 (2018), arXiv:1801.05235 [astro-ph.CO]

    work page Pith review arXiv 2018

  46. [46]

    A. M. Green and B. J. Kavanagh, J. Phys. G48, 043001 (2021), arXiv:2007.10722 [astro-ph.CO]

    work page arXiv 2021

  47. [47]

    Casanueva-Villarreal, N

    C. Casanueva-Villarreal, N. Padilla, P. B. Tissera, B. Liu, and V. Bromm, Astron. Astrophys.699, A49 (2025), arXiv:2505.10706 [astro-ph.CO]

    work page arXiv 2025

  48. [48]

    Byrnes, G

    C. Byrnes, G. Franciolini, T. Harada, P. Pani, and M. Sasaki, eds., Primordial Black Holes, Springer Series in Astrophysics and Cosmology (Springer, 2025)

    2025

  49. [49]

    Zumalacarregui and U

    M. Zumalacarregui and U. Seljak, Phys. Rev. Lett.121, 141101 (2018), arXiv:1712.02240 [astro- ph.CO]

    work page arXiv 2018

  50. [50]

    Mr´ oz et al.,No massive black holes in the Milky Way halo,Nature632(2024) 749 [2403.02386]

    P. Mr´ ozet al., Nature632, 749 (2024), arXiv:2403.02386 [astro-ph.GA]

    work page arXiv 2024

  51. [51]

    & Wright, D

    P. Mr´ ozet al., Astrophys. J. Suppl.280, 49 (2025), arXiv:2507.13794 [astro-ph.GA]

    work page arXiv 2025

  52. [52]

    Oguri, V

    M. Oguri, V. Takhistov, and K. Kohri, Phys. Lett. B847, 138276 (2023), arXiv:2208.05957 [astro- ph.CO]

    work page arXiv 2023

  53. [53]

    Oguri, J

    M. Oguri, J. M. Diego, N. Kaiser, P. L. Kelly, and T. Broadhurst, Phys. Rev. D97, 023518 (2018), arXiv:1710.00148 [astro-ph.CO]

    work page arXiv 2018

  54. [54]

    Andr´ es-Carcasona, A

    M. Andr´ es-Carcasona, A. J. Iovino, V. Vaskonen, H. Veerm¨ ae, M. Mart´ ınez, O. Pujol` as, and L. M. Mir, Phys. Rev. D110, 023040 (2024), arXiv:2405.05732 [astro-ph.CO]

    work page arXiv 2024

  55. [55]

    P. D. Serpico, V. Poulin, D. Inman, and K. Kohri, Phys. Rev. Res.2, 023204 (2020), arXiv:2002.10771 [astro-ph.CO]

    work page arXiv 2020

  56. [56]

    Agius, R

    D. Agius, R. Essig, D. Gaggero, F. Scarcella, G. Suczewski, and M. Valli, JCAP07, 003, arXiv:2403.18895 [hep-ph]

    work page arXiv

  57. [57]

    B. Carr, K. Kohri, Y. Sendouda, and J. Yokoyama, Rept. Prog. Phys.84, 116902 (2021), arXiv:2002.12778 [astro-ph.CO]

    work page arXiv 2021

  58. [58]

    B. Carr, A. J. Iovino, G. Perna, V. Vaskonen, and H. Veerm¨ ae 10.1007/s40766-026-00080-z (2026), arXiv:2601.06024 [astro-ph.CO]

    work page doi:10.1007/s40766-026-00080-z 2026

  59. [59]

    LOFAR, LOFAR2.0 White paper,https://www.lofar.eu/lofar2-0-documentation/(2023), [On- line; accessed 17-April-2026]

    2023

  60. [60]

    J. Wang, M. J. Norden, and P. Donker, (2025), arXiv:2503.02425 [astro-ph.IM]

    work page arXiv 2025

  61. [61]

    T. W. Shimwell et al., Astron. Astrophys.707, A198 (2026), arXiv:2602.15949 [astro-ph.GA]

    work page arXiv 2026

  62. [62]

    Jiang, R

    P. Jiang, R. Chen, H. Gan, J. Sun, B. Zhu, H. Li, W. Zhu, J. Wu, X. Chen, H. Zhang, and T. An, Astronomical Techniques and Instruments1, 84 (2024), arXiv:2408.12826 [astro-ph.IM]

    work page arXiv 2024

  63. [63]

    The BINGO Project I: Baryon Acoustic Oscillations from Integrated Neutral Gas Observations,

    E. Abdalla et al., Astron. Astrophys.664, A14 (2022), arXiv:2107.01633 [astro-ph.CO]

    work page arXiv 2022

  64. [64]

    M. V. dos Santos et al., Astron. Astrophys.681, A120 (2024), arXiv:2308.06805 [astro-ph.IM]

    work page arXiv 2024

  65. [65]

    Abdalla et al

    E. Abdalla et al. (2023) arXiv:2309.05099 [astro-ph.CO]

    work page arXiv 2023

  66. [66]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanim et al. (Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]

    work page Pith review arXiv 2020

  67. [67]

    Petroff et al., Mon

    E. Petroff et al., Mon. Not. Roy. Astron. Soc.447, 246 (2015), arXiv:1412.0342 [astro-ph.HE]

    work page arXiv 2015

  68. [68]

    C. W. James, J. X. Prochaska, J.-P. Macquart, F. O. North-Hickey, K. W. Bannister, and A. Dunning, Monthly Notices of the Royal Astronomical Society509, 4775–4802 (2021)

    2021

  69. [69]

    J. P. Macquart et al., Nature581, 391 (2020), arXiv:2005.13161 [astro-ph.CO]

    work page arXiv 2020

  70. [70]

    J. M. Shull, B. D. Smith, and C. W. Danforth, The Astrophysical Journal759, 23 (2012)

    2012

  71. [71]

    A. A. Meiksin, Rev. Mod. Phys.81, 1405 (2009), arXiv:0711.3358 [astro-ph]

    work page arXiv 2009

  72. [72]

    G. D. Becker, J. S. Bolton, M. G. Haehnelt, and W. L. W. Sargent, Mon. Not. Roy. Astron. Soc.410, 1096 (2011), arXiv:1008.2622 [astro-ph.CO]

    work page arXiv 2011

  73. [73]

    Bartelmann, Class

    M. Bartelmann, Class. Quant. Grav.27, 233001 (2010), arXiv:1010.3829 [astro-ph.CO]

    work page arXiv 2010

  74. [74]

    M. W. Sammons, J.-P. Macquart, R. D. Ekers, R. M. Shannon, H. Cho, J. X. Prochaska, A. T. Deller, and C. K. Day, Astrophys. J.900, 122 (2020), arXiv:2002.12533 [astro-ph.CO]. 16

    work page arXiv 2020

  75. [75]

    L. L. Sales, K. E. L. de Farias, A. R. Queiroz, J. R. L. Santos, R. A. Batista, A. R. M. Oliveira, L. F. Santana, C. A. Wuensche, T. Villela, and J. Vieira, (2025), arXiv:2507.06975 [astro-ph.CO]

    work page arXiv 2025

  76. [76]

    M. P. van Haarlem et al. (LOFAR), Astron. Astrophys.556, A2 (2013), arXiv:1305.3550 [astro-ph.IM]

    work page arXiv 2013

  77. [77]

    Chawla, A

    P. Chawla, A. Gopinath, N. Manaswini, C. Bassa, J. Hessels, V. Kondratiev, D. Michilli, and Z. Ple- unis, Mon. Not. Roy. Astron. Soc.544, 4079 (2025), arXiv:2509.01688 [astro-ph.HE]

    work page arXiv 2025

  78. [78]

    X. X. Zhang, R. Duan, V. Gajjar, H. Y. Zhang, P. Wang, C. H. Niu, D. Werthimer, J. Cobb, S. Y. Li, X. Pei, Y. Zhu, and D. Li, Research in Astronomy and Astrophysics23, 095023 (2023)

    2023

  79. [79]

    C. A. Wuensche et al., Astron. Astrophys.664, A15 (2022), arXiv:2107.01634 [astro-ph.IM]

    work page arXiv 2022

  80. [80]

    Sanidas et al., Astron

    S. Sanidas et al., Astron. Astrophys.626, A104 (2019), arXiv:1905.04977 [astro-ph.HE]

    work page arXiv 2019

Showing first 80 references.