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FAST Pulsar Database: II. Scattering profiles of 149 Pulsars

T0 review · 5 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read FAST L-band observations yield pulse-broadening timescales and scattering spectral indices for 122 pulsars, 93 of them first-time measurements.

desk verdict A potentially valuable scattering catalog is undermined by irreconcilable counts between the abstract and the text; the data deserve referee time, but only after a careful revision. read the letter →

arxiv 2506.14519 v2 pith:7AIHQCXN submitted 2025-06-17 astro-ph.HE astro-ph.GA

W. C. Jing , J. L. Han , C. Wang , P. F. Wang , T. Wang , N. N. Cai , J. Xu , Z. L. Yang
show 5 more authors
D. J. Zhou Yi Yan W. Q. Su X. Y. Gao L. Xie
This is my paper
classification astro-ph.HEastro-ph.GA PACS 97.60.Gb95.85.Bh
keywords pulsarsinterstellarscatteringpulsebroadeningspectralindexdispersionmeasureFASTtelescopeGalacticspiralarmspolarizationprofiles
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper aims to build a catalog of interstellar scattering properties from FAST L-band observations: for a large sample of pulsars it fits a pulse-broadening timescale at 1 GHz, $\tau_{\rm 1GHz}$, and a scattering spectral index $\alpha$ defined by $\tau_s(\nu)=\tau_{\rm 1GHz}\,\nu^{-\alpha}$. The draft text reports measurements for 122 pulsars, 93 of them first-time determinations, while the title and posted abstract say 149 pulsars and 113 first-time measurements; the tables list about 121 entries. The measurements matter because scattering broadens and delays pulsar pulses in a frequency-dependent way, and a homogeneous sample at high dispersion measures is exactly what tests electron-density fluctuation models of the Galactic disk. The paper further argues that aligning the front edge of a scattered profile at the 1/4 or 1/2 peak level gives better dispersion measures than conventional peak alignment, and that pulsars behind spiral arms show stronger scattering because of larger density fluctuations there.

What carries the argument

The machinery is the joint fitting of subband profiles. Three to five subbands across 1.0–1.5 GHz are each modeled as the convolution of a fixed multi-Gaussian intrinsic profile, an exponential thin-screen pulse-broadening function ${\rm PBF}(t)=\tau_s^{-1}\exp(-t/\tau_s)U(t)$, and rectangular smearing functions, with parameters refined by MCMC; the per-subband $\tau_s$ values are then fitted with the power law $\tau_s(\nu)=\tau_{\rm 1GHz}\,\nu^{-\alpha}$. A second iterative joint fit optimizes dispersion measure and scattering parameters together by aligning the main peak of the modeled intrinsic profiles, using the front-edge alignment at the 1/4 or 1/2 peak level as the starting DM. For PSR J1844$-$0310 and J1850$-$0026 the fixed intrinsic-profile assumption failed, and only after allowing frequency-evolving profile components did the fits give $\alpha\simeq4.2$ instead of about 5.7; the paper generalizes this warning to the rest of the catalog.

What would settle it

Fit the 32-subband FAST waterfall for a subset of the 122 pulsars twice: once with each subband's intrinsic-profile components forced to be identical and once with component amplitudes and widths free, then compare the resulting $\tau_{\rm 1GHz}$ and $\alpha$; if the differences exceed the quoted uncertainties for more than a few pulsars, the fixed-profile assumption is biasing the catalog.

Watch

Extended reading notes

Core claim

On the paper's own terms, FAST can detect the exponential pulse-broadening tail in enough subbands to determine both the pulse-broadening timescale at 1 GHz and the scattering spectral index for well over a hundred pulsars, most of them never measured before. The central relation is the power law $\tau_s(\nu)=\tau_{\rm 1GHz}\,\nu^{-\alpha}$, and the fitting model is the convolution $I(t)=S(t)\otimes D(t)\otimes {\rm PBF}(t)\otimes \Sigma G(t)$, where $\Sigma G(t)$ is an intrinsic profile made of at most three Gaussian components, ${\rm PBF}(t)=\tau_s^{-1}\exp(-t/\tau_s)\,U(t)$ is the thin-screen pulse-broadening function, and $S$ and $D$ are the sampling and intra-channel dispersion smearing functions. For the 29 pulsars with previous scattering measurements, the FAST timescales agree after interpolation to the reference frequency. In spiral-arm sectors the pulsars group by dispersion measure and the fluctuation parameter $\tilde F=(\tau_{\rm 1GHz}/0.48\,{\rm ms})({\rm DM}/100\,{\rm pc\,cm^{-3}})^{-2}$, which the authors read as different density-fluctuation properties in different arms; they also present polarization profiles for 41 scattered pulsars with flattened polarization-angle curves in the scattering tails.

Load-bearing premise

The load-bearing assumption is that, except for two pulsars, the intrinsic pulse profile keeps the same shape (a sum of at most three Gaussians) across the whole 1.0–1.5 GHz band, so all extra low-frequency broadening is attributed to scattering; if profile components evolve with frequency, the fitted $\tau_{\rm 1GHz}$ and $\alpha$ are biased.

Editorial extensions

If this is right

  • The catalog extends measured $\tau_{\rm 1GHz}$ and $\alpha$ values to high-dispersion-measure pulsars, where empirical $\tau$–DM relations are least constrained.
  • Front-edge DM alignment at the 1/4 or 1/2 peak level can replace peak alignment for scattered pulsars, improving DM-based distance estimates.
  • The grouping by dispersion measure and fluctuation parameter $\tilde F$ in spiral-arm sectors provides a rough distance indicator for pulsars behind identifiable arms.
  • The distribution of $\alpha$ around 4.0 supports Kolmogorov or Gaussian turbulence models, with outliers pointing to non-standard density spectra or finite screen sizes.
  • The polarization profiles confirm that scattering redistributes polarized emission into tails and flattens the polarization-angle curve, as earlier work predicted.

Reading between the lines

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

  • Because two of 122 pulsars needed frequency-evolving profile components, the true fraction of such pulsars may be larger; applying the same 32-subband residual test to the rest of the catalog would quantify the bias.
  • The front-edge DM-alignment rule is transferable to fast radio bursts, which are modeled with the same exponential pulse-broadening function and suffer the same peak-alignment DM bias.
  • If the $\tilde F$ groupings hold, the catalog can be combined with spiral-arm maps to localize strong scattering screens along the line of sight rather than treating scattering as an integrated path effect.
  • The posted abstract (149 pulsars, 113 first-time, 82 polarization profiles) must be reconciled with the draft text (122, 93, 41) before the database is cited by number; the final count will determine the catalog's reach.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

5 major / 5 minor

Summary. The paper presents FAST L-band (1.0–1.5 GHz) observations of pulsar pulse broadening. For each pulsar, the authors fit subband profiles with a model consisting of up to three Gaussian components convolved with an exponential pulse-broadening function, obtaining the pulse-broadening timescale at 1 GHz and the scattering spectral index. They also propose two DM-determination procedures, compare their scattering parameters with literature values, study the dependence of scattering on DM and spiral-arm location, and present subband polarization profiles. The central difficulty with the manuscript is that it contains two mutually inconsistent versions of the catalog: the arXiv abstract reports 149 pulsars, 68 GPPS discoveries, 113 first-time measurements, and 82 polarization profiles, while the full text reports 122 pulsars, 60 GPPS discoveries, 93 first-time measurements, and 41 polarization profiles; internal counts in Table 1, Figure A1, and the appendix text further disagree.

Significance. If the catalog size and composition were consistently defined, this would be a valuable contribution: FAST has the sensitivity to measure pulse-broadening timescales for a large sample, most of them for the first time, and the paper provides external validation against 29 literature pulsars as well as residual waterfall plots for the individual fits. The polarization profiles for 41 scattered pulsars are a useful addition. The claims are not circular: the scattering parameters are direct fits to the data and are checked against independent measurements. However, the unresolved version mismatch and the internal count inconsistencies mean that the actual contents of the claimed database are not currently specified, and the systematic uncertainty in the spectral index from the fixed intrinsic-profile assumption is not quantified. These issues must be resolved before the catalog can be assessed or used.

major comments (5)
  1. [Title/Abstract vs. Sections 3 and 4] The arXiv title and abstract state that 149 pulsars were detected, including 68 GPPS discoveries, 113 first-time scattering measurements, and 82 polarization profiles, while the full-text abstract, Section 3 ('In total, we have measured the scattering parameters for 122 pulsars'), and Section 4 state 122 pulsars, 60 GPPS discoveries, 93 first-time measurements, and 41 polarization profiles. The paper must present one unambiguous version of the catalog with consistent numbers in the title, abstract, body, tables, and figures.
  2. [Table 1 caption; Figure A1 caption; Appendix text] The counts within the full text also disagree: Table 1 is captioned 'Fitted scattering parameters for 121 pulsars', Figure A1 is captioned 'The observed and modeled scattering profiles for 120 pulsars', and the appendix text says 'Figure A1 presents the scattering profiles ... for 118 pulsars which have been well-fitted ... except for PSR J1844-0310 and J1850-0026'. Since 118 well-fitted pulsars plus the two exceptional cases give 120, none of these numbers matches the claimed 122. The authors should state exactly how many pulsars are in each table and each figure and ensure the totals are consistent.
  3. [Section 3, first paragraph] The statement that 'DM values derived from the two approaches are consistent within the 3σ error' is contradicted by entries in Table 1. For J1852+0031, DM1/4 = 752.0 ± 1.5 pc cm−3 and DM = 745.6 ± 1.3 pc cm−3 differ by about 3.2σ; for J1855+0422, 453.9 ± 0.9 and 449 ± 1 differ by about 3.6σ. The claim needs to be replaced by a quantitative comparison, and the outliers should be discussed.
  4. [Section 2.2.4 and Eq. (5)] The assumption that the intrinsic profile is a fixed sum of at most three Gaussians that does not evolve across 1.0–1.5 GHz is load-bearing for the central tau_1GHz and alpha measurements. The paper itself shows in Section 2.2.4 that for PSR J1844-0310 and PSR J1850-0026, allowing frequency-evolving components changes alpha from about 5.7 to about 4.2. Because the same fixed-profile assumption is used for the other pulsars, the reported statistical errors on alpha and tau_1GHz likely underestimate the systematic uncertainty. The authors should either demonstrate with a per-pulsar test that profile evolution is negligible, or add a systematic error term and state how it was estimated.
  5. [Section 3.1 and Table 2] The statement that FAST measurements are 'consistent with results in the literature' needs stronger qualification. In Table 2, PSR J1850-0026 has a literature tau of 46.5 ± 0.6 ms at 1000 MHz versus FAST 35.6 ± 0.4 ms, a difference of about 15σ, and alpha differs by 4.946 ± 0.002 versus 4.19 ± 0.04. The conclusion mentions 'a few exceptions', but the abstract says the values are consistent without this caveat. The paper should report the number of literature comparisons that agree within the quoted uncertainties and explicitly list the significant outliers.
minor comments (5)
  1. [Figure 4, 6, 7 captions] The captions contain the typo 'Frequncy' instead of 'Frequency'.
  2. [Table 2 note] The table note says 'column (9) scattering spectral index measured by FAST', but the table has only seven columns; the column numbering should be corrected.
  3. [Appendix text] The sentence describing Figure A1 is grammatically ambiguous: it says profiles are presented for 118 pulsars 'except for PSR J1844-0310 and J1850-0026', but those two are then said to be in Figure A2. Please clarify whether Figure A1 contains 118 or 120 pulsars and how the total of 122 is reached.
  4. [Section 3.4 and Figure A4] The text says 'The subband polarization profiles for another 40 pulsars ... are shown in Figure A4', while the abstract says 41 polarization profiles and Figure A4's caption says 41. Please make the count consistent and state whether J2052+4421g is included in the 41.
  5. [Table A1] Some subband timescales in Table A1 are non-monotonic with frequency (e.g., J1920+1340g: 270 ± 63 ms at 1088 MHz, 236 ± 23 ms at 1275 MHz, 230 ± 21 ms at 1383 MHz) or have very large asymmetric errors. A sentence explaining how such points are weighted in the power-law fit to obtain alpha and tau_1GHz would help the reader assess the reliability of those entries.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: scattering parameters are direct, externally validated fits; the arm-region F analysis is interpretive but not constructionally circular.

full rationale

The scattering parameters are obtained from direct convolution fits of FAST subband profiles (Eq. 5), followed by a power-law fit (Eq. 2) to the per-subband timescales; tau_1GHz and alpha are therefore derived from the data rather than defined in terms of the claims they support. The catalog is validated against external literature values (Table 2, Figure 8) and against independent 32-subband waterfall residuals (Section 2.2.3), so the measurements have external benchmarks outside the paper's fitted values. The DM-alignment method is benchmarked against the external 2-D fitting of Oswald et al. (2021), and the two exceptional pulsars are handled by explicitly modeling frequency-evolving components rather than hiding the degeneracy. The fluctuation parameter F (Eq. 6) is a deterministic rescaling of the same measured tau_1GHz and DM; using it to group pulsars in spiral-arm sectors is an interpretive re-description of measured data, not a prediction that reduces to its inputs by construction, and the arm boundaries come from external spiral-arm maps (Hou & Han 2014; Reid et al. 2019). No load-bearing self-citation or imported uniqueness theorem appears: GPPS discovery and polarization-calibration citations are procedural, not the source of the scattering results. The abstract/full-text discrepancies in pulsar counts (149 vs 122, 113 vs 93 first-time measurements, 82 vs 41 polarization profiles) are a real internal consistency and correctness problem, but they are not a circularity in the derivation chain.

Assumptions & free parameters 5 free parameters · 5 assumptions · 1 invented entities

The central measurements rest on standard but nontrivial modeling assumptions: an exponential thin-screen pulse broadening function, a fixed multi-Gaussian intrinsic profile, and a power-law frequency dependence. The DM and scattering parameters are fitted quantities, and the fluctuation parameter used for spiral arm grouping is defined from the same data, giving a mild self-referential element.

free parameters (5)
  • Intrinsic profile Gaussian component parameters (amplitudes, centers, widths, up to 3 per pulsar) = per pulsar; not tabulated
    Fitted to the highest-frequency subband and held fixed across the band; degeneracies between component shapes and tau_s can bias the scattering parameters.
  • Subband pulse-broadening timescale tau_s at central frequencies = in Table A1, e.g., J1841-0157: 10.29(9) ms at 1085 MHz
    The primary measured quantity, fit independently per subband with Eq. (5).
  • Scattering spectral index alpha and tau_1GHz = in Table 1, e.g., J1841-0157: tau_1GHz=14.44(6) ms, alpha=3.50(2)
    Derived from a power-law fit to the subband tau_s values; these are the headline results and inherit all model assumptions.
  • Dispersion measure (DM) = in Table 1, e.g., J1842-0153: DM=423.8(7) pc cm^-3
    Determined from front-edge alignment and then joint fitting; the final DM depends on the assumed intrinsic profile and PBF.
  • Scattered profile baseline offset = freely fitted per subband or skipped
    For profiles with long scattering tails, the baseline is uncertain and a fitted offset compensates; this can affect tau_s.
assumptions (5)
  • domain assumption Thin-screen exponential pulse broadening function PBF(t)=tau_s^-1 exp(-t/tau_s) U(t) (Eq. 1).
    Assumes a single thin scattering screen midway between pulsar and observer; for extended screens or non-exponential PBFs the inferred tau_s is biased.
  • domain assumption The intrinsic profile can be represented as a sum of at most three Gaussian components, identical across the 1.0-1.5 GHz band for all but two pulsars (Eq. 5, Section 2.2.1, 2.2.4).
    Enables joint fitting of subbands; frequency evolution of components, present in at least two pulsars, changes fitted alpha substantially, so the assumption may not hold generally.
  • domain assumption Pulse-broadening timescale follows a power law in frequency, tau_s(nu)=tau_1GHz nu^{-alpha} (Eq. 2).
    Standard form but an approximation; fitting over only 1.0-1.5 GHz cannot detect curvature or breaks.
  • domain assumption Distances and arm assignments rely on NE2001/YMW16 DM-based distance models and on the empirical Bhat et al. (2004) tau-DM relation (Section 3.2, 3.3, Eq. 3).
    These models carry systematic uncertainties; the spiral arm grouping and the fluctuation parameter interpretation depend on them.
  • domain assumption For scaling literature tau_s to 1 GHz when alpha is unknown, alpha=4.0 with uncertainty 0.6 is assumed (Section 3.2).
    Used for literature comparison; a wrong assumed alpha shifts the scaled tau_s.
invented entities (1)
  • Fluctuation parameter F (Eq. 6)
    purpose: To quantify density fluctuations in different spiral arm regions, defined as F = (tau_1GHz/0.48 ms)(DM/100)^-2.
    F is a rescaling of the measured tau_1GHz and DM; it carries no independent observable handle and is used to group pulsars into spiral arms, which is a post-hoc interpretation.

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Cite this review

Pith. "Pith review of FAST Pulsar Database: II. Scattering profiles of 149 Pulsars." pith.science (2026). https://pith.science/paper/7AIHQCXN

@misc{pith2026250614519,
  author       = {Pith},
  title        = {Pith review of: FAST Pulsar Database: II. Scattering profiles of 149 Pulsars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/7AIHQCXN}},
  note         = {Machine review of arXiv:2506.14519}
}
read the original abstract

The turbulent ionized interstellar medium diffracts radio waves and makes them propagate in multiple paths. The pulse-broadening observed at low frequencies results from the scattering effect of interstellar clouds of ionized gas. During the Galactic Plane Pulsar Snapshot (GPPS) survey and other projects by using the Five-hundred-meter Aperture Spherical radio Telescope (FAST), we detect the pulse-broadening for 149 pulsars in the radio frequency band between 1.0 and 1.5 GHz, including 68 newly discovered pulsars in the GPPS survey and 81 previously known pulsars. We find that a more accurate dispersion measure can be obtained from aligning the front edge of the scattered subband pulses at the 1/4 or 1/2 peak level for most pulsars with one dominant component in the intrinsic profile, and the best DM values from aligning the intrinsic profile components from the model-fitting. From the pulse profiles at a few subbands we derive the pulse-broadening timescale and the scattering spectral index. These scattering parameters are measured for the first time for 113 pulsars. For 36 pulsars with previously detected scattering features, our measurements of the pulse-broadening timescale are consistent with results in the literature. We find that pulsars behind spiral arms show a stronger scattering effect due to greater density fluctuations in the arm regions. With a properly derived dispersion measure and careful calibration, we also present polarization profiles for 82 pulsars in three subbands of FAST observations.

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Forward citations

Cited by 2 Pith papers

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Reference graph

Works this paper leans on

127 extracted references · 33 canonical work pages · cited by 2 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    lApd`x `L nixh lJ O VC0 1FgO !c du /PNa0E Mb ȱ l xJ SN Q !w ze `Iv 6Ke 2 ӻ Fd K`NapX- _0 !ػ` V + S &0 :n`DE0 t h# y:

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    arXiv 2021

  4. [4]

    G., Komesaroff , M

    Ables , J. G., Komesaroff , M. M., & Hamilton , P. A. 1970, , 6, 147

    1970

  5. [5]

    J., Cruz , A., Daniels , L., et al

    Aloisi , R. J., Cruz , A., Daniels , L., et al. 2019, , 875, 19, 10.3847/1538-4357/ab0d21

    work page doi:10.3847/1538-4357/ab0d21 2019

  6. [6]

    K., Bobra , A

    Alurkar , S. K., Bobra , A. D., & Slee , O. B. 1986, Australian Journal of Physics, 39, 433, 10.1071/PH860433

    work page doi:10.1071/ph860433 1986

  7. [7]

    C., Fonseca , E., McKee , J

    Andersen , B. C., Fonseca , E., McKee , J. W., et al. 2023, , 943, 57, 10.3847/1538-4357/aca485

    doi:10.3847/1538-4357/aca485 2023

  8. [8]

    B., Stovall , K., & Dowell , J

    Bansal , K., Taylor , G. B., Stovall , K., & Dowell , J. 2019, , 875, 146, 10.3847/1538-4357/ab0d8f

    work page doi:10.3847/1538-4357/ab0d8f 2019

Show all 127 references
  1. [9]

    Bernadich , M. C. i., Balakrishnan , V., Barr , E., et al. 2023, arXiv e-prints, arXiv:2308.16802, 10.48550/arXiv.2308.16802

    2023 doi arXiv

  2. [10]

    Bernadich , M. C. i., Venkatraman Krishnan , V., Champion , D. J., et al. 2024, arXiv e-prints, arXiv:2407.13593, 10.48550/arXiv.2407.13593

    2024 doi arXiv

  3. [11]

    S., Frail , D

    Bhakta , D., Deneva , J. S., Frail , D. A., et al. 2017, , 468, 2526, 10.1093/mnras/stx656

    2017 doi

  4. [12]

    Bhat , N. D. R., Cordes , J. M., Camilo , F., Nice , D. J., & Lorimer , D. R. 2004, , 605, 759, 10.1086/382680

    2004 doi

  5. [13]

    Bhat , N. D. R., Cordes , J. M., & Chatterjee , S. 2003, , 584, 782, 10.1086/345775

    2003 doi

  6. [14]

    Bhat , N. D. R., Tingay , S. J., & Knight , H. S. 2008, , 676, 1200, 10.1086/528735

    2008 doi

  7. [15]

    Bhat , N. D. R., Wayth , R. B., Knight , H. S., et al. 2007, , 665, 618, 10.1086/519444

    2007 doi

  8. [16]

    Bhattacharya , D., Wijers , R. A. M. J., Hartman , J. W., & Verbunt , F. 1992, , 254, 198

    1992

  9. [17]

    F., Macquart , J

    Brisken , W. F., Macquart , J. P., Gao , J. J., et al. 2010, , 708, 232, 10.1088/0004-637X/708/1/232

    2010 doi

  10. [18]

    M., Chatterjee , S., Johnston , S., & Demorest , P

    Camilo , F., Ransom , S. M., Chatterjee , S., Johnston , S., & Demorest , P. 2012, , 746, 63, 10.1088/0004-637X/746/1/63

    2012 doi

  11. [19]

    M., Gaensler , B

    Camilo , F., Ransom , S. M., Gaensler , B. M., & Lorimer , D. R. 2009, , 700, L34, 10.1088/0004-637X/700/1/L34

    2009 doi

  12. [20]

    M., Halpern , J

    Camilo , F., Ransom , S. M., Halpern , J. P., & Reynolds , J. 2007, , 666, L93, 10.1086/521826

    2007 doi

  13. [21]

    M., Halpern , J

    Camilo , F., Ransom , S. M., Halpern , J. P., & Roshi , D. A. 2021, , 917, 67, 10.3847/1538-4357/ac0720

    2021 doi

  14. [22]

    J., Ransom , S

    Champion , D. J., Ransom , S. M., Lazarus , P., et al. 2008, Science, 320, 1309, 10.1126/science.1157580

    2008 doi

  15. [23]

    L., Su , W

    Chen , X., Han , J. L., Su , W. Q., Yang , Z. L., & Zhou , D. J. 2023 a , Research in Astronomy and Astrophysics, 23, 104004, 10.1088/1674-4527/acd52b

    2023 doi

  16. [24]

    L., et al

    Chen , X., Yan , Y., Han , J. L., et al. 2023 b , Nature Astronomy, 7, 1235, 10.1038/s41550-023-02056-z

    2023 doi

  17. [25]

    M., Ananthakrishnan , S., & Dennison , B

    Cordes , J. M., Ananthakrishnan , S., & Dennison , B. 1984, , 309, 689, 10.1038/309689a0

    1984 doi

  18. [26]

    M., & Lazio , T

    Cordes , J. M., & Lazio , T. J. 1991, , 376, 123, 10.1086/170261

    1991 doi

  19. [27]

    M., & Lazio , T

    Cordes , J. M., & Lazio , T. J. W. 1997, , 475, 557, 10.1086/303569

    1997 doi

  20. [28]

    2001, , 549, 997, 10.1086/319442

    ---. 2001, , 549, 997, 10.1086/319442

    2001 doi

  21. [29]

    M., & Lazio , T

    Cordes , J. M., & Lazio , T. J. W. 2002, arXiv e-prints, astro. astro-ph/0207156

    2002 arXiv

  22. [30]

    2003, arXiv e-prints, astro

    ---. 2003, arXiv e-prints, astro. astro-ph/0301598

    2003 arXiv

  23. [31]

    M., Ocker , S

    Cordes , J. M., Ocker , S. K., & Chatterjee , S. 2022, , 931, 88, 10.3847/1538-4357/ac6873

    2022 doi

  24. [32]

    M., & Rickett , B

    Cordes , J. M., & Rickett , B. J. 1998, , 507, 846, 10.1086/306358

    1998 doi

  25. [33]

    M., Weisberg , J

    Cordes , J. M., Weisberg , J. M., & Boriakoff , V. 1985, , 288, 221, 10.1086/162784

    1985 doi

  26. [34]

    M., Wharton , R

    Cordes , J. M., Wharton , R. S., Spitler , L. G., Chatterjee , S., & Wasserman , I. 2016, arXiv e-prints, arXiv:1605.05890. 1605.05890

    2016 arXiv

  27. [35]

    M., Wolszczan , A., Dewey , R

    Cordes , J. M., Wolszczan , A., Dewey , R. J., Blaskiewicz , M., & Stinebring , D. R. 1990, , 349, 245, 10.1086/168310

    1990 doi

  28. [36]

    Cronyn , W. M. 1970, Science, 168, 1453, 10.1126/science.168.3938.1453

    1970

  29. [37]

    Demorest , P. B. 2011, , 416, 2821, 10.1111/j.1365-2966.2011.19230.x

    2011

  30. [38]

    S., Cordes , J

    Deneva , J. S., Cordes , J. M., & Lazio , T. J. W. 2009, , 702, L177, 10.1088/0004-637X/702/2/L177

    2009 doi

  31. [39]

    A., et al

    Desvignes , G., Cognard , I., Smith , D. A., et al. 2022, , 667, A79, 10.1051/0004-6361/202244171

    2022 doi

  32. [40]

    C., et al

    Dexter , J., Deller , A., Bower , G. C., et al. 2017, , 471, 3563, 10.1093/mnras/stx1777

    2017 doi

  33. [41]

    K., & Taylor , G

    Eftekhari , T., Stovall , K., Dowell , J., Schinzel , F. K., & Taylor , G. B. 2016, , 829, 62, 10.3847/0004-637X/829/2/62

    2016 doi

  34. [42]

    W., Clarke , T

    Ellingson , S. W., Clarke , T. E., Craig , J., et al. 2013, , 768, 136, 10.1088/0004-637X/768/2/136

    2013 doi

  35. [43]

    2024, , 271, 49, 10.3847/1538-4365/ad27d6

    Fonseca , E., Pleunis , Z., Breitman , D., et al. 2024, , 271, 49, 10.3847/1538-4365/ad27d6

    2024 doi

  36. [44]

    A., & Clifton , T

    Frail , D. A., & Clifton , T. R. 1989, , 336, 854, 10.1086/167056

    1989 doi

  37. [45]

    Gautam , T., Ridolfi , A., Freire , P. C. C., et al. 2022, , 664, A54, 10.1051/0004-6361/202243062

    2022 doi

  38. [46]

    2016, , 462, 2587, 10.1093/mnras/stw1724

    Geyer , M., & Karastergiou , A. 2016, , 462, 2587, 10.1093/mnras/stw1724

    2016 doi

  39. [47]

    I., et al

    Geyer , M., Karastergiou , A., Kondratiev , V. I., et al. 2017, , 470, 2659, 10.1093/mnras/stx1151

    2017 doi

  40. [48]

    2021, , 505, 4468, 10.1093/mnras/stab1501

    Geyer , M., Serylak , M., Abbate , F., et al. 2021, , 505, 4468, 10.1093/mnras/stab1501

    2021 doi

  41. [49]

    L., Wang , C., Wang , P

    Han , J. L., Wang , C., Wang , P. F., et al. 2021, Research in Astronomy and Astrophysics, 21, 107, 10.1088/1674-4527/21/5/107

    2021 doi

  42. [50]

    L., Zhou , D

    Han , J. L., Zhou , D. J., Wang , C., et al. 2024, Research in Astronomy and Astrophysics, submitted

    2024

  43. [51]

    2024, , 527, 5183, 10.1093/mnras/stad3561

    He , Q., & Shi , X. 2024, , 527, 5183, 10.1093/mnras/stad3561

    2024 doi

  44. [52]

    2025, arXiv e-prints, arXiv:2502.09158

    He , Q., Shi , X., & Li , G. 2025, arXiv e-prints, arXiv:2502.09158. 2502.09158

    2025 arXiv

  45. [53]

    Hessels , J. W. T., Spitler , L. G., Seymour , A. D., et al. 2019, , 876, L23, 10.3847/2041-8213/ab13ae

    2019 doi

  46. [54]

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

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

    2004 doi

  47. [55]

    G., & Han , J

    Hou , L. G., & Han , J. L. 2014, , 569, A125, 10.1051/0004-6361/201424039

    2014 doi

  48. [56]

    2020, Research in Astronomy and Astrophysics, 20, 064, 10.1088/1674-4527/20/5/64

    Jiang , P., Tang , N.-Y., Hou , L.-G., et al. 2020, Research in Astronomy and Astrophysics, 20, 064, 10.1088/1674-4527/20/5/64

    2020 doi

  49. [57]

    C., Han , J

    Jing , W. C., Han , J. L., Hong , T., et al. 2023, , 523, 4949, 10.1093/mnras/stad1782

    2023 doi

  50. [58]

    R., et al

    Johnston , S., Kramer , M., Lorimer , D. R., et al. 2006, , 373, L6, 10.1111/j.1745-3933.2006.00232.x

    2006

  51. [59]

    Johnston , S., & Romani , R. W. 2003, , 590, L95, 10.1086/376826

    2003 doi

  52. [61]

    M., et al

    Kerr , M., Hobbs , G., Shannon , R. M., et al. 2014, , 445, 320, 10.1093/mnras/stu1716

    2014 doi

  53. [62]

    Kirsten , F., Bhat , N. D. R., Meyers , B. W., et al. 2019, , 874, 179, 10.3847/1538-4357/ab0c05

    2019 doi

  54. [63]

    M., Hamilton , P

    Komesaroff , M. M., Hamilton , P. A., & Ables , J. G. 1972, Australian Journal of Physics, 25, 759, 10.1071/PH720759

    1972 doi

  55. [64]

    A., Pushkarev , A

    Koryukova , T. A., Pushkarev , A. B., Plavin , A. V., & Kovalev , Y. Y. 2022, , 515, 1736, 10.1093/mnras/stac1898

    2022 doi

  56. [65]

    1994, , 107, 527

    Kramer , M. 1994, , 107, 527

    1994

  57. [66]

    P., Zakharenko , V

    Kravtsov , I. P., Zakharenko , V. V., Ulyanov , O. M., et al. 2022, , 512, 4324, 10.1093/mnras/stab3369

    2022 doi

  58. [67]

    A., Joshi , B

    Krishnakumar , M. A., Joshi , B. C., & Manoharan , P. K. 2017, , 846, 104, 10.3847/1538-4357/aa7af2

    2017 doi

  59. [68]

    A., Maan , Y., Joshi , B

    Krishnakumar , M. A., Maan , Y., Joshi , B. C., & Manoharan , P. K. 2019, , 878, 130, 10.3847/1538-4357/ab20c5

    2019 doi

  60. [69]

    A., Mitra , D., Naidu , A., Joshi , B

    Krishnakumar , M. A., Mitra , D., Naidu , A., Joshi , B. C., & Manoharan , P. K. 2015, , 804, 23, 10.1088/0004-637X/804/1/23

    2015 doi

  61. [70]

    D., & Izvekova , V

    Kuz'min , A. D., & Izvekova , V. A. 1993, , 260, 724, 10.1093/mnras/260.4.724

    1993 doi

  62. [71]

    D., Kondrat'ev , V

    Kuz'min , A. D., Kondrat'ev , V. I., Kostyuk , S. V., et al. 2002, Astronomy Letters, 28, 251, 10.1134/1.1467260

    2002 doi

  63. [72]

    D., Losovskii , B

    Kuz'min , A. D., Losovskii , B. Y., & Lapaev , K. A. 2007, Astronomy Reports, 51, 615, 10.1134/S1063772907080021

    2007 doi

  64. [73]

    D., & Losovsky , B

    Kuzmin , A. D., & Losovsky , B. Y. 2007, Astronomical and Astrophysical Transactions, 26, 597, 10.1080/10556790701610282

    2007 doi

  65. [74]

    D., Dai , S., et al

    Lazarevi \'c , S., Filipovi \'c , M. D., Dai , S., et al. 2024, , 41, e032, 10.1017/pasa.2024.13

    2024 doi

  66. [75]

    Lazio , T. J. W., Cordes , J. M., de Bruyn , A. G., & Macquart , J. P. 2004, , 48, 1439, 10.1016/j.newar.2004.09.039

    2004 doi

  67. [76]

    C., & Jokipii , J

    Lee , L. C., & Jokipii , J. R. 1975 a , , 196, 695, 10.1086/153458

    1975 doi

  68. [77]

    1975 b , , 201, 532, 10.1086/153916

    ---. 1975 b , , 201, 532, 10.1086/153916

    1975 doi

  69. [78]

    2013, , 434, 69, 10.1093/mnras/stt989

    Lewandowski , W., Dembska , M., Kijak , J., & Kowali \'n ska , M. 2013, , 434, 69, 10.1093/mnras/stt989

    2013 doi

  70. [79]

    2015 a , , 449, 1570, 10.1093/mnras/stv385

    Lewandowski , W., Kowali \'n ska , M., & Kijak , J. 2015 a , , 449, 1570, 10.1093/mnras/stv385

    2015 doi

  71. [80]

    2015 b , , 454, 2517, 10.1093/mnras/stv2159

    Lewandowski , W., Ro \.z ko , K., Kijak , J., Bhattacharyya , B., & Roy , J. 2015 b , , 454, 2517, 10.1093/mnras/stv2159

    2015 doi

  72. [81]

    H., & Han , J

    Li , X. H., & Han , J. L. 2003, , 410, 253, 10.1051/0004-6361:20031190

    2003 doi

  73. [82]

    R., & Lyne , A

    L \"o hmer , O., Kramer , M., Mitra , D., Lorimer , D. R., & Lyne , A. G. 2001, , 562, L157, 10.1086/338324

    2001 doi

  74. [83]

    2004, , 425, 569, 10.1051/0004-6361:20035881

    L \"o hmer , O., Mitra , D., Gupta , Y., Kramer , M., & Ahuja , A. 2004, , 425, 569, 10.1051/0004-6361:20035881

    2004 doi

  75. [84]

    E., Dai , S., Johnston , S., & Barr , E

    Lower , M. E., Dai , S., Johnston , S., & Barr , E. D. 2024, , 967, L16, 10.3847/2041-8213/ad4866

    2024 doi

  76. [85]

    2017, , 840, L15, 10.3847/2041-8213/aa6f03

    Main , R., van Kerkwijk , M., Pen , U.-L., Mahajan , N., & Vanderlinde , K. 2017, , 840, L15, 10.3847/2041-8213/aa6f03

    2017 doi

  77. [86]

    N., Hobbs , G

    Manchester , R. N., Hobbs , G. B., Teoh , A., & Hobbs , M. 2005, , 129, 1993, 10.1086/428488

    2005 doi

  78. [87]

    W., Tremblay , S

    Meyers , B. W., Tremblay , S. E., Bhat , N. D. R., et al. 2017, , 851, 20, 10.3847/1538-4357/aa8bba

    2017 doi

  79. [88]

    2006, Science in China: Physics, Mechanics and Astronomy, 49, 129, 10.1007/s11433-006-0129-9

    Nan , R. 2006, Science in China: Physics, Mechanics and Astronomy, 49, 129, 10.1007/s11433-006-0129-9

    2006 doi

  80. [89]

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

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

    2011 doi

  81. [90]

    J., Altiere , E., Bogdanov , S., et al

    Nice , D. J., Altiere , E., Bogdanov , S., et al. 2013, , 772, 50, 10.1088/0004-637X/772/1/50

    2013 doi

  82. [91]

    T., Johnston , S., Kramer , M., et al

    O'Brien , J. T., Johnston , S., Kramer , M., et al. 2008, , 388, L1, 10.1111/j.1745-3933.2008.00481.x

    2008

  83. [92]

    K., Cordes , J

    Ocker , S. K., Cordes , J. M., & Chatterjee , S. 2020, , 897, 124, 10.3847/1538-4357/ab98f9

    2020 doi

  84. [93]

    2021, , 911, 102, 10.3847/1538-4357/abeb6e

    ---. 2021, , 911, 102, 10.3847/1538-4357/abeb6e

    2021 doi

  85. [94]

    K., Cordes , J

    Ocker , S. K., Cordes , J. M., Chatterjee , S., & Gorsuch , M. R. 2022, arXiv e-prints, arXiv:2203.16716. 2203.16716

    2022 arXiv

  86. [95]

    I., Ord , S

    Oronsaye , S. I., Ord , S. M., Bhat , N. D. R., et al. 2015, , 809, 51, 10.1088/0004-637X/809/1/51

    2015 doi

  87. [96]

    S., Karastergiou , A., Posselt , B., et al

    Oswald , L. S., Karastergiou , A., Posselt , B., et al. 2021, , 504, 1115, 10.1093/mnras/stab980

    2021 doi

  88. [97]

    Parent , E., Sewalls , H., Freire , P. C. C., et al. 2022, , 924, 135, 10.3847/1538-4357/ac375d

    2022 doi

  89. [98]

    T., Possenti , A., Esposito , P., et al

    Pennucci , T. T., Possenti , A., Esposito , P., et al. 2015, , 808, 81, 10.1088/0004-637X/808/1/81

    2015 doi

  90. [99]

    A., McConnell , D

    Ramachandran , R., Mitra , D., Deshpande , A. A., McConnell , D. M., & Ables , J. G. 1997, , 290, 260, 10.1093/mnras/290.2.260

    1997 doi

  91. [100]

    J., Menten , K

    Reid , M. J., Menten , K. M., Brunthaler , A., et al. 2019, , 885, 131, 10.3847/1538-4357/ab4a11

    2019 doi

  92. [101]

    Rickett , B. J. 1977, , 15, 479, 10.1146/annurev.aa.15.090177.002403

    1977

  93. [102]

    1990, , 28, 561, 10.1146/annurev.aa.28.090190.003021

    ---. 1990, , 28, 561, 10.1146/annurev.aa.28.090190.003021

    1990

  94. [103]

    Scheuer , P. A. G. 1968, , 218, 920, 10.1038/218920a0

    1968 doi

  95. [104]

    2023, , 522, 1071, 10.1093/mnras/stad508

    Sengar , R., Bailes , M., Balakrishnan , V., et al. 2023, , 522, 1071, 10.1093/mnras/stad508

    2023 doi

  96. [105]

    C., Krishnakumar , M

    Singha , J., Joshi , B. C., Krishnakumar , M. A., et al. 2024, , 535, 1184, 10.1093/mnras/stae2405

    2024 doi

  97. [106]

    B., Dulk , G

    Slee , O. B., Dulk , G. A., & Otrupcek , R. E. 1980, , 4, 100, 10.1017/S1323358000018968

    1980 doi

  98. [107]

    V., & Shishov , V

    Smirnova , T. V., & Shishov , V. I. 2010, Astronomy Reports, 54, 139, 10.1134/S106377291002006X

    2010 doi

  99. [108]

    G., Lee , K

    Spitler , L. G., Lee , K. J., Eatough , R. P., et al. 2014, , 780, L3, 10.1088/2041-8205/780/1/L3

    2014 doi

  100. [109]

    Staelin , D. H. 1970, , 226, 69, 10.1038/226069a0

    1970 doi

  101. [110]

    Q., Han , J

    Su , W. Q., Han , J. L., Wang , P. F., et al. 2023, arXiv e-prints, arXiv:2305.16754, 10.48550/arXiv.2305.16754

    2023 doi arXiv

  102. [111]

    P., Joshi , B

    Surnis , M. P., Joshi , B. C., McLaughlin , M. A., et al. 2019, , 870, 8, 10.3847/1538-4357/aaee7f

    2019 doi

  103. [112]

    Sutton , J. M. 1971, , 155, 51, 10.1093/mnras/155.1.51

    1971 doi

  104. [113]

    H., & Cordes , J

    Taylor , J. H., & Cordes , J. M. 1993, , 411, 674, 10.1086/172870

    1993 doi

  105. [114]

    2004, , 152, 129, 10.1086/383187

    van Straten , W. 2004, , 152, 129, 10.1086/383187

    2004 doi

  106. [115]

    2011, , 28, 1, 10.1071/AS10021

    van Straten , W., & Bailes , M. 2011, , 28, 1, 10.1071/AS10021

    2011 doi

  107. [116]

    2012, Astronomical Research and Technology, 9, 237, 10.48550/arXiv.1205.6276

    van Straten , W., Demorest , P., & Oslowski , S. 2012, Astronomical Research and Technology, 9, 237, 10.48550/arXiv.1205.6276

    2012 doi arXiv

  108. [117]

    Vo \^u te , J. L. L., Kouwenhoven , M. L. A., van Haren , P. C., et al. 2002, , 385, 733, 10.1051/0004-6361:20020123

    2002 doi

  109. [118]

    F., Han , J

    Wang , P. F., Han , J. L., Xu , J., et al. 2023, Research in Astronomy and Astrophysics, 23, 104002, 10.1088/1674-4527/acea1f

    2023 doi

  110. [119]

    Q., Wang , J

    Wang , S. Q., Wang , J. B., Hobbs , G., et al. 2020, , 897, 8, 10.3847/1538-4357/ab9302

    2020 doi

  111. [120]

    J., Bailes , M., et al

    Wongphechauxsorn , J., Champion , D. J., Bailes , M., et al. 2023, arXiv e-prints, arXiv:2310.14008, 10.48550/arXiv.2310.14008

    2023 doi arXiv

  112. [121]

    2022, Science China Physics, Mechanics, and Astronomy, 65, 129704, 10.1007/s11433-022-2033-2

    Xu , J., Han , J., Wang , P., & Yan , Y. 2022, Science China Physics, Mechanics, and Astronomy, 65, 129704, 10.1007/s11433-022-2033-2

    2022 doi

  113. [122]

    2017, , 835, 2, 10.3847/1538-4357/835/1/2

    Xu , S., & Zhang , B. 2017, , 835, 2, 10.3847/1538-4357/835/1/2

    2017 doi

  114. [123]

    M., Tremblay , S

    Xue , M., Ord , S. M., Tremblay , S. E., et al. 2019, , 36, e025, 10.1017/pasa.2019.19

    2019 doi

  115. [124]

    L., Zhou , D

    Yan , Y., Han , J. L., Zhou , D. J., et al. 2024, , 965, 25, 10.3847/1538-4357/ad2e9c

    2024 doi

  116. [125]

    F., & Han , J

    Yan , Y., Wang , P. F., & Han , J. L. 2023, , 523, 5207, 10.1093/mnras/stad1775

    2023 doi

  117. [126]

    M., Manchester , R

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

    2017 doi

  118. [127]

    Young , O., & Lam , M. T. 2024, , 962, 131, 10.3847/1538-4357/ad1ce7

    2024 doi

  119. [128]

    V., Vasylieva , I

    Zakharenko , V. V., Vasylieva , I. Y., Konovalenko , A. A., et al. 2013, , 431, 3624, 10.1093/mnras/stt470

    2013 doi

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