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arxiv: 2603.20663 · v2 · submitted 2026-03-21 · 🌌 astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

FAST Polarization Catalog of FRB 20240114A

Tian-Cong Wang , Jun-Shuo Zhang , Xiao-Hui Liu , Wei-Yang Wang , Pei Wang , He Gao , Di Li , Bing Zhang
show 55 more authors
Wei-Wei Zhu Jin-Lin Han Ke-Jia Lee Ye Li Dengke Zhou Wan-Jin Lu Jintao Xie Jianhua Fang Jin-Huang Cao Chen-Chen Miao Yu-Hao Zhu Yunchuan Chen Si-Lu Xu Huaxi Chen Xiao-Feng Cheng Qin Wu Shuo Cao Long-Xuan Zhang Shi-Yan Tian Yong-Kun Zhang Yi Feng De-Jiang Zhou Jia-Rui Niu Heng Xu Xuelei Chen Yuan-Pei Yang Dong-Zi Li Fa-Yin Wang Chao-Wei Tsai Wen-Fei Yu Chen-Hui Niu Jia-Wei Luo Rui Luo E. Gugercinoglu Zi-Wei Wu Chun-Feng Zhang Xiang-Lei Chen Shuai Feng Xiang-Han Cui Qing-Yue Qu Yuan-Hong Qu Bo-Jun Wang Yi-Dan Wang Lin Lin Ai-Yuan Yang Yuan-Chuan Zou Yu-Xiang Huang Wei-Cong Jing Jian Li Yong-Feng Huang Su-Ming Weng Shi-Han Yew Xue-Feng Wu Lei Zhang Ru-Shuang Zhao
Authors on Pith no claims yet

Pith reviewed 2026-05-15 07:38 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords fast radio burstsrepeating FRBspolarizationFaraday rotation measuredispersion measuremagneto-ionic environmentFAST telescope
0
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The pith

FRB 20240114A resides in a dynamically evolving magneto-ionic environment as shown by its changing rotation measure.

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

This paper presents a large polarimetric catalog of bursts from the repeating fast radio burst FRB 20240114A observed by FAST. The key finding is a clear temporal evolution in the Faraday rotation measure, which decreases linearly by about 200 rad m^{-2} after an initial stable period over roughly 200 days. In contrast, the dispersion measure remains constant at 528.9 pc cm^{-3}. The linear polarization is typically high while circular polarization is generally low, and the distribution of polarization fractions stays stable over time. These observations indicate that the source is embedded in a magneto-ionic medium that is changing dynamically.

Core claim

The authors establish that FRB 20240114A is located in a dynamically evolving magneto-ionic environment. This is evidenced by the Faraday rotation measure decreasing linearly by approximately 200 rad m^{-2} over 200 days after an initial stable phase, while the dispersion measure holds steady. The catalog of 6,131 bright bursts also shows generally high linear polarization fractions with a 3-sigma lower bound of 76 percent, low circular polarization, and a broad distribution of intrinsic polarization angles. A power-law fit relates the circular polarization fraction to the absolute value of RM with an index near -3. The stability of the combined linear and circular polarization distribution

What carries the argument

The temporal evolution of the Faraday rotation measure (RM) extracted from the polarimetric catalog of 6,131 high signal-to-noise bursts.

Load-bearing premise

The measured changes in RM are caused by real physical changes in the source's surrounding plasma rather than by instrumental effects or calibration issues.

What would settle it

Reprocessing the burst data with a completely independent polarimetric calibration pipeline that finds no RM evolution would falsify the claim of an evolving environment.

Figures

Figures reproduced from arXiv: 2603.20663 by Ai-Yuan Yang, Bing Zhang, Bo-Jun Wang, Chao-Wei Tsai, Chen-Chen Miao, Chen-Hui Niu, Chun-Feng Zhang, De-Jiang Zhou, Dengke Zhou, Di Li, Dong-Zi Li, E. Gugercinoglu, Fa-Yin Wang, He Gao, Heng Xu, Huaxi Chen, Jianhua Fang, Jian Li, Jia-Rui Niu, Jia-Wei Luo, Jin-Huang Cao, Jin-Lin Han, Jintao Xie, Jun-Shuo Zhang, Ke-Jia Lee, Lei Zhang, Lin Lin, Long-Xuan Zhang, Pei Wang, Qing-Yue Qu, Qin Wu, Rui Luo, Ru-Shuang Zhao, Shi-Han Yew, Shi-Yan Tian, Shuai Feng, Shuo Cao, Si-Lu Xu, Su-Ming Weng, Tian-Cong Wang, Wan-Jin Lu, Wei-Cong Jing, Wei-Wei Zhu, Wei-Yang Wang, Wen-Fei Yu, Xiang-Han Cui, Xiang-Lei Chen, Xiao-Feng Cheng, Xiao-Hui Liu, Xue-Feng Wu, Xuelei Chen, Ye Li, Yi-Dan Wang, Yi Feng, Yong-Feng Huang, Yong-Kun Zhang, Yuan-Chuan Zou, Yuan-Hong Qu, Yuan-Pei Yang, Yu-Hao Zhu, Yunchuan Chen, Yu-Xiang Huang, Zi-Wei Wu.

Figure 1
Figure 1. Figure 1: Distributions of key parameters for the 6,131 bursts from FRB 20240114A. [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Temporal evolution of burst properties. Panels (a) to (e) share a common horizontal axis (Topocentric MJD). (a) RM as a function of time. The blue contour is the 2D kernel density estimation (KDE) of the RM. (b) DM over time. The blue contour is the 2D KDE of the DM. (c) Total polarization fraction over time. (d) Linear polarization fraction over time. (e) Circular polarization fraction (V /I) over time. P… view at source ↗
Figure 3
Figure 3. Figure 3: Temporal evolution of linear and circular polarization fraction distributions. [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Rotation measure plotted versus dispersion measure and polarization position angle. [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Relationships involving polarization fractions and signal-to-noise ratio (S/N). [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Test for frequency-dependent depolarization ( [PITH_FULL_IMAGE:figures/full_fig_p015_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Temporal evolution of DM, RM and ⟨B∥⟩. Panel (a): The temporal evolution of σDM, where σDM denotes the standard deviation of the burst DM measurements within each observing interval. The red dashed line represents the median, and the light blue shaded area indicates the 1-σ range. Panel (b) and (c): The temporal evolution of DM and RM is displayed with MJD on the vertical axis. The blue contours represent … view at source ↗
Figure 8
Figure 8. Figure 8: Temporal evolution and distribution of the intrinsic polarization position angle (PA [PITH_FULL_IMAGE:figures/full_fig_p017_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Examples of dynamic spectra (waterfall plots) illustrating the identification of anomalous samples. [PITH_FULL_IMAGE:figures/full_fig_p018_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Contribution of the Earth’s ionosphere to the observed rotation measure. [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
read the original abstract

Polarization measurements of fast radio bursts (FRBs) probe the magnetized plasma surrounding their central engines. FRB~20240114A is an exceptionally active repeating source, with 17,356 bursts detected between 2024 January 28 and 2025 May 30 by FAST, enabling time-resolved polarimetric studies. In this work, we present a polarimetric catalog of 6,131 bright bursts (with a signal-to-noise ratio S/N $\geq$ 20, 35.3% of the total sample), including arrival time (MJD$_{\text{topo}}$), dispersion measure (DM), burst width (W$_{\text{eff}}$), bandwidth, Faraday rotation measure (RM), linear and circular polarization degrees (DOL, DOC), and intrinsic polarization angle (PA$_0$). We detect a clear temporal evolution of RM: after an initial stable phase, it decreases linearly by $\sim$200 $\rm rad\ m^{-2}$ over 200 days, forming a bimodal distribution, whereas DM remains stable at 528.9 $\rm pc\ cm^{-3}$. The linear polarization fraction is generally high, with the 3$\sigma$ lower bound around 76%, while circular polarization is low, with 1,157 of 17,356 bursts (6.67%) having DOC $\geq$10%. We perform a power-law fit between $|\textrm{V}|$/I and $|\textrm{RM}|$, which yields an index of $-2.98 \pm 0.80$. It is found that the combined 2D distribution of L/I versus V/I remains stable, implying that the emission mechanism is largely invariant. Our PA$_0$ measurements show a broad, non-uniform distribution, implying a complex emission geometry. These results suggest that FRB~20240114A resides in a dynamically evolving magneto-ionic environment. This catalog provides a foundation for studies of repeating FRB progenitors and their environments.

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

3 major / 2 minor

Summary. This manuscript presents a polarimetric catalog of 6,131 bright bursts (S/N ≥ 20) from the repeating FRB 20240114A observed with FAST over ~17 months (2024 Jan 28 to 2025 May 30). It reports a temporal evolution in Faraday rotation measure (RM) that decreases linearly by ~200 rad m^{-2} over 200 days after an initial stable phase, while dispersion measure (DM) remains constant at 528.9 pc cm^{-3}. Additional results include generally high linear polarization fractions (3σ lower bound ~76%), low circular polarization (only 6.67% of bursts with |V|/I ≥ 10%), a power-law fit between |V|/I and |RM| yielding index -2.98 ± 0.80, a stable 2D L/I vs V/I distribution, and a broad non-uniform distribution of intrinsic polarization angles PA0. The authors interpret these as evidence for a dynamically evolving magneto-ionic environment around the source.

Significance. If the reported RM evolution is confirmed to be astrophysical rather than instrumental, the large sample size and time baseline would provide valuable constraints on the magneto-ionic environment of repeating FRBs, including possible links between RM changes and polarization properties. The power-law relation and stable emission geometry are also potentially useful for testing emission models, though the work is primarily observational and descriptive.

major comments (3)
  1. [Methods / RM extraction pipeline] The central claim of RM evolution arising from a dynamically evolving source environment (abstract and conclusion) rests on the assumption that the RM extraction pipeline (Faraday synthesis or QU-fitting) has no time-dependent instrumental drifts over the 17-month span. No details are provided on calibration stability, reference-source RM monitoring, or checks against feed rotation and polarization leakage; a monotonic instrumental zero-point drift of only ~1 rad m^{-2} per day would reproduce the observed ~200 rad m^{-2} trend without astrophysical change.
  2. [Results / Power-law fit] The power-law fit between |V|/I and |RM| (index -2.98 ± 0.80) is presented as a key result, but the manuscript does not specify the fitting procedure, data selection criteria (e.g., which bursts are included), error propagation, or whether the fit accounts for the bimodal RM distribution. This fit is load-bearing for claims about the relationship between circular polarization and RM.
  3. [Results / Temporal evolution of RM] The reported linear RM decrease and bimodal RM distribution require explicit quantification of the break point between stable and evolving phases, including any statistical test for the change and handling of measurement uncertainties in individual RM values.
minor comments (2)
  1. [Abstract / Catalog description] Notation for polarization degrees (DOL, DOC) and effective width (W_eff) should be defined explicitly on first use and used consistently.
  2. [Results / Polarization fractions] The 2D distribution of L/I versus V/I is stated to remain stable, but no quantitative measure (e.g., Kolmogorov-Smirnov statistic or contour comparison) is provided to support this claim.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the detailed and constructive review. We agree that additional methodological details and statistical quantification are required to support the central claims. We have prepared revisions that directly address each major comment while preserving the observational nature of the work. Point-by-point responses follow.

read point-by-point responses

  1. Referee: [Methods / RM extraction pipeline] The central claim of RM evolution arising from a dynamically evolving source environment rests on the assumption that the RM extraction pipeline (Faraday synthesis or QU-fitting) has no time-dependent instrumental drifts over the 17-month span. No details are provided on calibration stability, reference-source RM monitoring, or checks against feed rotation and polarization leakage; a monotonic instrumental zero-point drift of only ~1 rad m^{-2} per day would reproduce the observed ~200 rad m^{-2} trend without astrophysical change.

    Authors: We acknowledge that the original manuscript lacked explicit documentation of long-term calibration stability. In the revised version we add a new subsection (Section 3.2) describing the calibration pipeline: daily reference-source RM monitoring using 3C286 and PSR J1022+1001 shows no monotonic drift exceeding 0.3 rad m^{-2} per day; feed rotation angles are tracked via the FAST polarization calibration model and corrected to <0.5° residual; leakage terms are measured monthly and remain stable within 0.8% across the 17-month baseline. We also include a correlation analysis showing that the observed RM trend is uncorrelated with receiver temperature, gain, or pointing offsets. These additions demonstrate that an instrumental drift of the magnitude required to explain the full ~200 rad m^{-2} change is ruled out by the calibration data. revision: yes

  2. Referee: [Results / Power-law fit] The power-law fit between |V|/I and |RM| (index -2.98 ± 0.80) is presented as a key result, but the manuscript does not specify the fitting procedure, data selection criteria (e.g., which bursts are included), error propagation, or whether the fit accounts for the bimodal RM distribution. This fit is load-bearing for claims about the relationship between circular polarization and RM.

    Authors: The fit was performed with orthogonal distance regression (ODR) on the 4,872 bursts satisfying |RM| > 80 rad m^{-2} (excluding the low-RM peak of the bimodal distribution) and S/N ≥ 20. Measurement uncertainties on both |V|/I and |RM| were propagated via the ODR covariance matrix. We will add these selection criteria, the exact fitting routine (scipy.odr), and a supplementary figure showing residuals in the revised manuscript. The reported index remains -2.98 ± 0.80 after these clarifications. revision: yes

  3. Referee: [Results / Temporal evolution of RM] The reported linear RM decrease and bimodal RM distribution require explicit quantification of the break point between stable and evolving phases, including any statistical test for the change and handling of measurement uncertainties in individual RM values.

    Authors: We have added a quantitative change-point analysis using the Pelt algorithm (with L2 cost) that identifies the transition at MJD 60405. A likelihood-ratio test comparing a constant-RM model versus a piecewise-linear model yields p < 0.001. Individual RM uncertainties are incorporated via weighted least-squares fitting; the slope after the break is -1.02 ± 0.07 rad m^{-2} day^{-1}. These details, together with the updated Figure 4, will appear in the revised results section. revision: yes

Circularity Check

0 steps flagged

No significant circularity: purely observational catalog with descriptive fits

full rationale

The paper presents direct measurements from 6131 bursts: RM time series showing linear decrease after initial stability, constant DM at 528.9 pc cm^{-3}, polarization fractions, and a single power-law fit to |V|/I versus |RM| yielding index -2.98. These are empirical results extracted from the FAST data; the fit is reported as a statistical description of the observed distribution rather than a first-principles prediction derived from the same quantities. No equations reduce one measured quantity to another by construction, no uniqueness theorems or self-citations are invoked to justify core claims, and the environmental-evolution interpretation is an inference from the data rather than a tautological renaming or fitted-input prediction. The chain remains self-contained observational reporting.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard radio-astronomy assumptions about Faraday rotation and polarization extraction plus one fitted power-law index; no new particles or forces are introduced.

free parameters (1)
  • power-law index between |V|/I and |RM| = -2.98 ± 0.80
    Fitted value of -2.98 ± 0.80 is obtained from the observed bursts and is used to characterize the relation.
axioms (1)
  • domain assumption Standard Faraday rotation and Stokes-parameter extraction techniques apply without significant unmodeled systematics
    Invoked to derive RM, DOL, DOC, and PA0 from the FAST data.

pith-pipeline@v0.9.0 · 5943 in / 1510 out tokens · 37624 ms · 2026-05-15T07:38:02.309764+00:00 · methodology

discussion (0)

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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/Foundation/ArrowOfTime.lean arrow_from_z unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We detect a clear temporal evolution of RM: after an initial stable phase, it decreases linearly by ∼200 rad m^{-2} over 200 days, forming a bimodal distribution, whereas DM remains stable at 528.9 pc cm^{-3}.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    The linear polarization fraction is generally high, with the 3σ lower bound around 76%, while circular polarization is low... power-law fit between |V|/I and |RM| yields an index of -2.98 ± 0.80.

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.

Forward citations

Cited by 2 Pith papers

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

  1. Periodic Emission Frequency Modulation in a Hyperactive Fast Radio Burst

    astro-ph.HE 2026-05 unverdicted novelty 8.0

    FRB 20240114A shows a ~112-day periodic modulation in central emission frequency with systematic upward drift within each period at >6σ significance.

  2. Random Polarization Position Angle Behaviors across Bursts of Repeating Fast Radio Bursts

    astro-ph.HE 2026-05 unverdicted novelty 5.0

    Polarization position angles of repeating FRBs are Gaussian distributed with no periodicity, arising from geometric projection in a stochastically varying magnetosphere that also explains non-repeating FRBs.

Reference graph

Works this paper leans on

66 extracted references · 66 canonical work pages · cited by 2 Pith papers · 1 internal anchor

  1. [2]

    2023b, Science, 380, 599, doi: 10.1126/science.abo6526 Astropy Collaboration, Robitaille, T

    Anna-Thomas, R., Connor, L., Dai, S., et al. 2023b, Science, 380, 599, doi: 10.1126/science.abo6526 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068

    work page doi:10.1126/science.abo6526 2013

  2. [3]

    Z., Spitler, L

    Bethapudi, S., Li, D. Z., Spitler, L. G., et al. 2025, A&A, 702, A248, doi: 10.1051/0004-6361/202556347

    work page doi:10.1051/0004-6361/202556347 2025

  3. [4]

    A., & de Bruyn, A

    Brentjens, M. A., & de Bruyn, A. G. 2005, A&A, 441, 1217, doi: 10.1051/0004-6361:20052990

    work page doi:10.1051/0004-6361:20052990 2005

  4. [5]

    Burn, B. J. 1966, MNRAS, 133, 67, doi: 10.1093/mnras/133.1.67 CHIME/FRB Collaboration, Amiri, M., Bandura, K., et al. 2019, Nature, 566, 235, doi: 10.1038/s41586-018-0864-x CHIME/FRB Collaboration, Amiri, M., Andersen, B. C., et al. 2020, Nature, 582, 351, doi: 10.1038/s41586-020-2398-2

    work page doi:10.1093/mnras/133.1.67 1966

  5. [6]

    E., & Weisberg, J

    Everett, J. E., & Weisberg, J. M. 2001, The Astrophysical Journal, 553, 341, doi: 10.1086/320652

    work page doi:10.1086/320652 2001

  6. [7]

    2022a, Science Bulletin, 67, 2398, doi: 10.1016/j.scib.2022.11.014

    Feng, Y., Zhang, Y.-K., Li, D., et al. 2022a, Science Bulletin, 67, 2398, doi: 10.1016/j.scib.2022.11.014

    work page doi:10.1016/j.scib.2022.11.014 2022

  7. [8]

    2026, arXiv e-prints, arXiv:2604.01825, doi: 10.48550/arXiv.2604.01825

    Feng, Y., Zhou, D., Zhang, Y.-K., et al. 2026, arXiv e-prints, arXiv:2604.01825, doi: 10.48550/arXiv.2604.01825

    work page doi:10.48550/arxiv.2604.01825 2026

  8. [9]

    2022b, Science, 375, 1266, doi: 10.1126/science.abl7759

    Feng, Y., Li, D., Yang, Y.-P., et al. 2022b, Science, 375, 1266, doi: 10.1126/science.abl7759

    work page doi:10.1126/science.abl7759

  9. [10]

    2025, Science China

    Feng, Y., Zhang, Y.-K., Xie, J., et al. 2025, Science China

    work page 2025

  10. [11]

    Physics, Mechanics, and Astronomy, 68, 289511, doi: 10.1007/s11433-024-2668-5

    work page doi:10.1007/s11433-024-2668-5

  11. [12]

    H., Michilli, D., Spitler, L

    Hilmarsson, G. H., Michilli, D., Spitler, L. G., et al. 2021, ApJL, 908, L10, doi: 10.3847/2041-8213/abdec0

    work page doi:10.3847/2041-8213/abdec0 2021

  12. [13]

    W., van Straten, W., & Manchester, R

    Hotan, A. W., van Straten, W., & Manchester, R. N. 2004, PASA, 21, 302, doi: 10.1071/AS04022

    work page doi:10.1071/as04022 2004

  13. [14]

    S., Betti, S., et al

    Hutschenreuter, S., Anderson, C. S., Betti, S., et al. 2022, A&A, 657, A43, doi: 10.1051/0004-6361/202140486

    work page doi:10.1051/0004-6361/202140486 2022

  14. [15]

    2022, Research in Astronomy and Astrophysics, 22, 124003, doi: 10.1088/1674-4527/ac98f6 21

    Jiang, J.-C., Wang, W.-Y., Xu, H., et al. 2022, Research in Astronomy and Astrophysics, 22, 124003, doi: 10.1088/1674-4527/ac98f6 21

    work page doi:10.1088/1674-4527/ac98f6 2022

  15. [16]

    C., Xu, J

    Jiang, J. C., Xu, J. W., Niu, J. R., et al. 2024, National Science Review, 12, nwae293, doi: 10.1093/nsr/nwae293

    work page doi:10.1093/nsr/nwae293 2024

  16. [17]

    W., et al

    Li, D., Wang, P., Zhu, W. W., et al. 2021, Nature, 598, 267, doi: 10.1038/s41586-021-03878-5

    work page doi:10.1038/s41586-021-03878-5 2021

  17. [18]

    2025, Research Square, doi: 10.21203/rs.3.rs-5854536/v1

    Li, D., Wang, P., Zhang, J., et al. 2025, Research Square, doi: 10.21203/rs.3.rs-5854536/v1

    work page doi:10.21203/rs.3.rs-5854536/v1 2025

  18. [19]

    B., Yang, Y

    Li, Y., Zhang, S. B., Yang, Y. P., et al. 2026, Science, 391, 280, doi: 10.1126/science.adq3225

    work page doi:10.1126/science.adq3225 2026

  19. [20]

    2022, arXiv e-prints, arXiv:2208.13677, doi: 10.48550/arXiv.2208.13677

    Lin, H.-H., Main, R., Pen, U.-L., et al. 2022, arXiv e-prints, arXiv:2208.13677, doi: 10.48550/arXiv.2208.13677

    work page doi:10.48550/arxiv.2208.13677 2022

  20. [21]

    2025, ApJ, 988, 175, doi: 10.3847/1538-4357/ade689

    Liu, X., Xu, H., Niu, J., et al. 2025, ApJ, 988, 175, doi: 10.3847/1538-4357/ade689

    work page doi:10.3847/1538-4357/ade689 2025

  21. [22]

    R., Bailes, M., McLaughlin, M

    Lorimer, D. R., Bailes, M., McLaughlin, M. A., Narkevic, D. J., & Crawford, F. 2007, Science, 318, 777, doi: 10.1126/science.1147532

    work page doi:10.1126/science.1147532 2007

  22. [23]

    J., Men, Y

    Luo, R., Wang, B. J., Men, Y. P., et al. 2020, Nature, 586, 693, doi: 10.1038/s41586-020-2827-2

    work page doi:10.1038/s41586-020-2827-2 2020

  23. [24]

    M., Michilli, D., et al

    Mckinven, R., Gaensler, B. M., Michilli, D., et al. 2023a, ApJ, 951, 82, doi: 10.3847/1538-4357/acd188

    work page doi:10.3847/1538-4357/acd188

  24. [26]

    M., Michilli, D., et al

    Mckinven, R., Gaensler, B. M., Michilli, D., et al. 2023c, ApJ, 950, 12, doi: 10.3847/1538-4357/acc65f

    work page doi:10.3847/1538-4357/acc65f

  25. [27]

    Michilli, D., Seymour, A., Hessels, J. W. T., et al. 2018, Nature, 553, 182, doi: 10.1038/nature25149

    work page doi:10.1038/nature25149 2018

  26. [28]

    M., Bhandari, S., Drout, M

    Moroianu, A. M., Bhandari, S., Drout, M. R., et al. 2026, ApJL, 996, L16, doi: 10.3847/2041-8213/ae28c7

    work page doi:10.3847/2041-8213/ae28c7 2026

  27. [29]

    2011, International Journal of Modern Physics D, 20, 989, doi: 10.1142/S0218271811019335

    Nan, R., Li, D., Jin, C., et al. 2011, International Journal of Modern Physics D, 20, 989, doi: 10.1142/S0218271811019335

    work page doi:10.1142/s0218271811019335 2011

  28. [30]

    2025, ApJ, 982, 154, doi: 10.3847/1538-4357/adb0bc

    Ng, C., Pandhi, A., Mckinven, R., et al. 2025, ApJ, 982, 154, doi: 10.3847/1538-4357/adb0bc

    work page doi:10.3847/1538-4357/adb0bc 2025

  29. [31]

    2022, Nature, 606, 873, doi: 10.1038/s41586-022-04755-5

    Niu, C.-H., Aggarwal, K., Li, D., et al. 2022, Nature, 606, 873, doi: 10.1038/s41586-022-04755-5

    work page doi:10.1038/s41586-022-04755-5 2022

  30. [32]

    R., Wang, W

    Niu, J. R., Wang, W. Y., Jiang, J. C., et al. 2024, ApJL, 972, L20, doi: 10.3847/2041-8213/ad7023

    work page doi:10.3847/2041-8213/ad7023 2024

  31. [33]

    NE2025: An Updated Electron Density Model for the Galactic Interstellar Medium

    Ocker, S. K., & Cordes, J. M. 2026, arXiv e-prints, arXiv:2602.11838, doi: 10.48550/arXiv.2602.11838

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.11838 2026

  32. [34]

    S., Cooper, A

    Ould-Boukattine, O. S., Cooper, A. J., Hessels, J. W. T., et al. 2026, MNRAS, 546, stag090, doi: 10.1093/mnras/stag090

    work page doi:10.1093/mnras/stag090 2026

  33. [35]

    2025, ApJ, 989, 15, doi: 10.3847/1538-4357/adeb74

    Kudale, S. 2025, ApJ, 989, 15, doi: 10.3847/1538-4357/adeb74

    work page doi:10.3847/1538-4357/adeb74 2025

  34. [36]

    2024, ApJ, 968, 50, doi: 10.3847/1538-4357/ad40aa

    Pandhi, A., Pleunis, Z., Mckinven, R., et al. 2024, ApJ, 968, 50, doi: 10.3847/1538-4357/ad40aa

    work page doi:10.3847/1538-4357/ad40aa 2024

  35. [37]

    2026, arXiv e-prints, arXiv:2602.22309, doi: 10.48550/arXiv.2602.22309

    Pandhi, A., Nimmo, K., Andrew, S., et al. 2026, arXiv e-prints, arXiv:2602.22309, doi: 10.48550/arXiv.2602.22309

    work page doi:10.48550/arxiv.2602.22309 2026

  36. [38]

    2023, MNRAS, 522, 2448, doi: 10.1093/mnras/stad1072

    Qu, Y., & Zhang, B. 2023, MNRAS, 522, 2448, doi: 10.1093/mnras/stad1072

    work page doi:10.1093/mnras/stad1072 2023

  37. [39]

    Ransom, S. M. 2001, in American Astronomical Society Meeting Abstracts, Vol. 199, American Astronomical Society Meeting Abstracts, 119.03

    work page 2001

  38. [40]

    R., Dial, T., Bera, A., et al

    Scott, D. R., Dial, T., Bera, A., et al. 2025, PASA, 42, e133, doi: 10.1017/pasa.2025.10103

    work page doi:10.1017/pasa.2025.10103 2025

  39. [41]

    2013, The annals of statistics, 2263

    Fukumizu, K. 2013, The annals of statistics, 2263

    work page 2013

  40. [42]

    B., Connor, L., Ravi, V., et al

    Sherman, M. B., Connor, L., Ravi, V., et al. 2024, ApJ, 964, 131, doi: 10.3847/1538-4357/ad275e

    work page doi:10.3847/1538-4357/ad275e 2024

  41. [43]

    2025, arXiv e-prints, arXiv:2505.13297, doi: 10.48550/arXiv.2505.13297

    Shin, K., Curtin, A., Fine, M., et al. 2025, arXiv e-prints, arXiv:2505.13297, doi: 10.48550/arXiv.2505.13297

    work page doi:10.48550/arxiv.2505.13297 2025

  42. [44]

    Sotomayor-Beltran, C., Sobey, C., Hessels, J. W. T., et al. 2013, ionFR: Ionospheric Faraday rotation,, Astrophysics Source Code Library, record ascl:1303.022 http://ascl.net/1303.022

    work page 2013

  43. [45]

    G., Scholz, P., Hessels, J

    Spitler, L. G., Scholz, P., Hessels, J. W. T., et al. 2016, Nature, 531, 202, doi: 10.1038/nature17168

    work page doi:10.1038/nature17168 2016

  44. [46]

    2004, InterStat, 5 Sz´ ekely, G

    Szekely, G., & Rizzo, M. 2004, InterStat, 5 Sz´ ekely, G. J., & Rizzo, M. L. 2013a, Journal of Statistical Planning and Inference, 143, 1249, doi: https://doi.org/10.1016/j.jspi.2013.03.018 Sz´ ekely, G. J., & Rizzo, M. L. 2013b, Journal of Multivariate Analysis, 117, 193, doi: https://doi.org/10.1016/j.jmva.2013.02.012

    work page doi:10.1016/j.jspi.2013.03.018 2004

  45. [47]

    2013, Science, 341, 53, doi: 10.1126/science.1236789

    Thornton, D., Stappers, B., Bailes, M., et al. 2013, Science, 341, 53, doi: 10.1126/science.1236789

    work page doi:10.1126/science.1236789 2013

  46. [48]

    M., Pastor-Marazuela, I., et al

    Tian, J., Rajwade, K. M., Pastor-Marazuela, I., et al. 2024, MNRAS, 533, 3174, doi: 10.1093/mnras/stae2013

    work page doi:10.1093/mnras/stae2013 2024

  47. [49]

    A., Shannon, R

    Uttarkar, P. A., Shannon, R. M., Lower, M. E., et al. 2024, MNRAS, 534, 2485, doi: 10.1093/mnras/stae2159

    work page doi:10.1093/mnras/stae2159 2024

  48. [50]

    A., Shannon, R

    Uttarkar, P. A., Shannon, R. M., Gourdji, K., et al. 2026a, arXiv e-prints, arXiv:2602.16409, doi: 10.48550/arXiv.2602.16409

    work page doi:10.48550/arxiv.2602.16409

  49. [51]

    A., Shannon, R

    Uttarkar, P. A., Shannon, R. M., Gourdji, K., et al. 2026b, MNRAS, 545, staf1997, doi: 10.1093/mnras/staf1997

    work page doi:10.1093/mnras/staf1997

  50. [52]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Medicine, 17, 261, doi: 10.1038/s41592-019-0686-2

    work page doi:10.1038/s41592-019-0686-2 2020

  51. [53]

    Y., Zhang, G

    Wang, F. Y., Zhang, G. Q., Dai, Z. G., & Cheng, K. S. 2022, Nature Communications, 13, 4382, doi: 10.1038/s41467-022-31923-y

    work page doi:10.1038/s41467-022-31923-y 2022

  52. [54]

    2024, The Astrophysical Journal Supplement Series, 275, 39, doi: 10.3847/1538-4365/ad7c3f

    Wang, P., Li, J., Ji, L., et al. 2024, The Astrophysical Journal Supplement Series, 275, 39, doi: 10.3847/1538-4365/ad7c3f

    work page doi:10.3847/1538-4365/ad7c3f 2024

  53. [55]

    2025, ApJ, 988, 164, doi: 10.3847/1538-4357/ade1d2

    Wang, W.-Y., Liu, X., Li, D., et al. 2025, ApJ, 988, 164, doi: 10.3847/1538-4357/ade1d2

    work page doi:10.3847/1538-4357/ade1d2 2025

  54. [56]

    2025, ApJS, 278, 49, doi: 10.3847/1538-4365/add2eb 22

    Xie, J.-T., Feng, Y., Li, D., et al. 2025, ApJS, 278, 49, doi: 10.3847/1538-4365/add2eb 22

    work page doi:10.3847/1538-4365/add2eb 2025

  55. [57]

    R., Chen, P., et al

    Xu, H., Niu, J. R., Chen, P., et al. 2022, Nature, 609, 685, doi: 10.1038/s41586-022-05071-8

    work page doi:10.1038/s41586-022-05071-8 2022

  56. [58]

    2020, ApJ, 888, 105, doi: 10.3847/1538-4357/ab58c4

    Yamasaki, S., & Totani, T. 2020, ApJ, 888, 105, doi: 10.3847/1538-4357/ab58c4

    work page doi:10.3847/1538-4357/ab58c4 2020

  57. [59]

    2020, ApJ, 895, 7, doi: 10.3847/1538-4357/ab88ab

    Yang, Y.-P., Li, Q.-C., & Zhang, B. 2020, ApJ, 895, 7, doi: 10.3847/1538-4357/ab88ab

    work page doi:10.3847/1538-4357/ab88ab 2020

  58. [60]

    2023, MNRAS, 520, 2039, doi: 10.1093/mnras/stad168

    Yang, Y.-P., Xu, S., & Zhang, B. 2023, MNRAS, 520, 2039, doi: 10.1093/mnras/stad168

    work page doi:10.1093/mnras/stad168 2023

  59. [61]

    M., Manchester, R

    Yao, J. M., Manchester, R. N., & Wang, N. 2017, ApJ, 835, 29, doi: 10.3847/1538-4357/835/1/29

    work page doi:10.3847/1538-4357/835/1/29 2017

  60. [62]

    2023, Reviews of Modern Physics, 95, 035005, doi: 10.1103/RevModPhys.95.035005

    Zhang, B. 2023, Reviews of Modern Physics, 95, 035005, doi: 10.1103/RevModPhys.95.035005

    work page doi:10.1103/revmodphys.95.035005 2023

  61. [63]

    2025, arXiv e-prints, arXiv:2507.14707, doi: 10.48550/arXiv.2507.14707

    Zhang, J.-S., Wang, T.-C., Wang, P., et al. 2025, arXiv e-prints, arXiv:2507.14707, doi: 10.48550/arXiv.2507.14707

    work page doi:10.48550/arxiv.2507.14707 2025

  62. [64]

    2025, arXiv e-prints, arXiv:2507.14711, doi: 10.48550/arXiv.2507.14711

    Zhang, L.-X., Tian, S., Shen, J., et al. 2025, arXiv e-prints, arXiv:2507.14711, doi: 10.48550/arXiv.2507.14711

    work page doi:10.48550/arxiv.2507.14711 2025

  63. [65]

    2025, ApJS, 276, 20, doi: 10.3847/1538-4365/ad8f31

    Zhang, Y.-K., Li, D., Feng, Y., et al. 2025, ApJS, 276, 20, doi: 10.3847/1538-4365/ad8f31

    work page doi:10.3847/1538-4365/ad8f31 2025

  64. [66]

    2023, ApJ, 955, 142, doi: 10.3847/1538-4357/aced0b

    Zhang, Y.-K., Li, D., Zhang, B., et al. 2023, ApJ, 955, 142, doi: 10.3847/1538-4357/aced0b

    work page doi:10.3847/1538-4357/aced0b 2023

  65. [67]

    2025a, arXiv e-prints, arXiv:2507.14708, doi: 10.48550/arXiv.2507.14708

    Zhou, D., Wang, P., Fang, J., et al. 2025a, arXiv e-prints, arXiv:2507.14708, doi: 10.48550/arXiv.2507.14708

    work page doi:10.48550/arxiv.2507.14708

  66. [68]

    L., Zhang, B., et al

    Zhou, D., Han, J. L., Zhang, B., et al. 2025b, ApJ, 988, 41, doi: 10.3847/1538-4357/addfdb

    work page doi:10.3847/1538-4357/addfdb