{"id":"76705e2c-eb14-432f-86ad-b894ce33f7ee","arxiv_id":"2506.14519","paper_version":2,"verdict":"REJECT","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"high","formal_verification":"none","parameter_count":5,"one_line_summary":"Pulse-broadening timescales and scattering spectral indices are measured for 122 pulsars from FAST observations, 93 of them for the first time.","lead":"This paper reports new measurements of how interstellar gas smears out the radio pulses of over a hundred pulsars observed with China's FAST telescope, many measured for the first time. The results refine how dispersion measures are derived from scattered profiles and suggest stronger turbulence behind spiral arms.","discovery_kind":"extension","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The posted abstract and the full text describe different catalogs (149 vs 122 pulsars, 82 vs 41 polarization profiles), so the central database claim is not currently well-defined.","rationale":"I identify the abstract/body numerical inconsistency as the most load-bearing concern because it attacks the definition of the central result: the catalog size, the number of new measurements, and the number of polarization profiles. Until these numbers are reconciled, no reader can tell what was actually measured, so the paper cannot be accepted in its current form. The reader's weaker-assumption concern about the fixed intrinsic profile (Eq. 5) is also important and independently worrying; the two exceptional pulsars in §2.2.4 show profile evolution can shift alpha from about 5.7 to about 4.2. However, that concern is about the accuracy of individual catalog entries and could in principle be addressed by re-analysis, whereas the inconsistency is a property of the submitted manuscript itself and is immediately verifiable. I therefore keep the reader's REJECT verdict unchanged, while endorsing the recommendation that the numbers be aligned and the fixed-profile assumption be tested in a revision.","tokens_in":42191,"tokens_out":8665,"duration_ms":95458,"concrete_test":"Count the rows in Table 1 and Table A1 and the entries in Table A2 / Figure A4, and compare with the abstract and the Conclusions. If Table 1 contains 122 pulsars and Table A2 contains 41 polarization profiles, then the 149/82 abstract is superseded and a corrected title/abstract would resolve the inconsistency. If the tables contain 149 rows or 82 polarization profiles, the body is missing data and the catalog is incomplete. In either case, recompute the 'first-time' counts (93 vs 113) using the literature compilation in §3.1 to see which claims are supported. This check requires only the submitted tables and can be done by any referee.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The manuscript's central claim is a database of scattering parameters, but the paper does not present a single coherent version of that database. The arXiv abstract and title state 149 pulsars, 68 GPPS-discovered pulsars, 113 first-time scattering measurements, and 82 polarization profiles. The full-text draft dated 2025-09-13 states 122 pulsars, 60 GPPS discoveries, 93 first-time measurements, and 41 polarization profiles, and the Conclusions repeat the 122/93 numbers. Internal counts also disagree: Table 1 is captioned for 121 pulsars, Figure A1 for 120, and the appendix text says 118 well-fitted pulsars plus two exceptional cases. A reader cannot determine how many pulsars are in the catalog, which values are new, or how many polarization profiles are being released. These are not cosmetic differences; the size and composition of the catalog is the headline result. As submitted, the central claim is internally inconsistent and the database is not unambiguously specified.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","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.","tokens_in":42413,"tokens_out":5145,"duration_ms":52918,"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":[{"comment":"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.","section":"Title/Abstract vs. Sections 3 and 4"},{"comment":"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.","section":"Table 1 caption; Figure A1 caption; Appendix text"},{"comment":"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.","section":"Section 3, first paragraph"},{"comment":"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.","section":"Section 2.2.4 and Eq. (5)"},{"comment":"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.","section":"Section 3.1 and Table 2"}],"minor_comments":[{"comment":"The captions contain the typo 'Frequncy' instead of 'Frequency'.","section":"Figure 4, 6, 7 captions"},{"comment":"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.","section":"Table 2 note"},{"comment":"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.","section":"Appendix text"},{"comment":"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.","section":"Section 3.4 and Figure A4"},{"comment":"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.","section":"Table A1"}],"recommendation":"major_revision","confidential_remarks":"The discrepancy between the arXiv abstract (149 pulsars, 113 first-time measurements, 82 polarization profiles) and the full text (122 pulsars, 93 first-time measurements, 41 polarization profiles) is so large that I initially wondered whether the submitted text was a different paper. The issue appears to be a version mismatch rather than a deliberate misrepresentation, but it must be resolved before the catalog can be evaluated. The paper is otherwise within scope for a database-focused journal such as RAA. I recommend major revision, not rejection, because the inconsistencies and the systematic-error question are fixable within the manuscript's scope."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Colleague,\n\nQuick take on Jing et al., \"FAST Pulsar Database: II.\" The underlying work is a large catalog of pulse-broadening timescales and spectral indices for over a hundred pulsars from FAST, and the body text reports 93 first-time measurements with good external validation against the literature for 29 previously published pulsars. That is a real contribution to the pulsar/ISM community. They also provide 2-D waterfall validation plots for every pulsar, which is more than most catalog papers do, and they handle the two pulsars with frequency-evolving profiles explicitly rather than forcing them into the standard template. The DM-alignment discussion is practical and useful.\n\nThe problem is not the data—it is the manuscript's self-consistency. The arXiv abstract says 149 pulsars, 113 first-time measurements, and 82 polarization profiles. The full text (dated September 2025) says 122, 93, and 41. That is not a rounding error; the size of the catalog is the headline result. The internal counts do not agree either: Table 1 is captioned for 121 pulsars, Figure A1 says 120, and the appendix text says 118 well-fitted pulsars plus two exceptions. Since this is a database paper, the reader cannot tell which numbers to trust. The \"consistent within 3 sigma\" claim about the two DM estimates is also overstated—PSR J1855+0422, for example, differs by roughly 4 sigma.\n\nThe bigger methodological assumption—fixed Gaussian intrinsic profiles across 1.0–1.5 GHz—is handled honestly for the two known exceptions, but it remains a possible source of bias for the rest. I would call that a moderate concern rather than a fatal one; the waterfall residuals look good, and this is a normal caveat for this type of analysis.\n\nMy verdict: as submitted, I would not accept this. The inconsistency is load-bearing, and a database paper that cannot state its own size is not publishable. But the data are real, the validation is thorough, and the fix is mechanical: align the abstract with the body, correct the internal counts, and temper the DM claim. I would send it to a serious referee rather than desk reject, because the underlying catalog is exactly what the subfield needs. It is a heavy-revision situation, not a rejection of the science.\n\nFor your reading group: maybe, as a lesson in how version control can bury a good dataset.","headline":"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.","tokens_in":43027,"tokens_out":3814,"would_cite":false,"duration_ms":37000,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":["97.60.Gb","95.85.Bh"],"model":"deepseek-v4-flash","headline":"FAST L-band observations yield pulse-broadening timescales and scattering spectral indices for 122 pulsars, 93 of them first-time measurements.","keywords":["pulsars","interstellar scattering","pulse broadening","scattering spectral index","dispersion measure","FAST telescope","Galactic spiral arms","polarization profiles"],"falsifier":"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.","tokens_in":41992,"feed_emoji":"📡","tokens_out":10623,"duration_ms":99167,"temperature":0.7,"pith_summary":"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.","feed_headline":"FAST publishes scattering catalog for 122 pulsars","feed_subtitle":"Broadening timescales and spectral indices, most measured for the first time, trace turbulence in spiral arms.","key_machinery":"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.","core_discovery":"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.","pith_inferences":["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."],"forward_implications":["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."],"supporting_citations":[{"why":"It supplies the direct subband-profile fitting method and the main literature comparison sample.","marker":"Oswald et al. 2021"},{"why":"It provides the empirical log(τs)–DM relation in Equation 3 and a multi-frequency scattering collection used for comparison.","marker":"Bhat et al. 2004"},{"why":"It provides the empirical τ1GHz–DM formula in Equation 4 and the observed scatter that the FAST data are checked against.","marker":"Cordes et al. 2022"},{"why":"It introduced simultaneous fitting of intrinsic profile, τ1GHz, and DM with α fixed to 4, which this paper extends by leaving α free.","marker":"Nice et al. 2013"},{"why":"It established the practice of allowing frequency-evolving profile components in scattering fits, used here for the two exceptional pulsars.","marker":"Lewandowski et al. 2015b"},{"why":"It predicted the flattening of polarization-angle curves in scattered tails that the paper's polarization profiles confirm.","marker":"Li & Han 2003"},{"why":"It describes the GPPS survey that discovered the new pulsars.","marker":"Han et al. 2021"},{"why":"It specifies the FAST polarization calibration procedure used for the subband polarization profiles.","marker":"Wang et al. 2023"},{"why":"It provides the low α measurement for PSR J1913+11025 that the paper re-fits with a two-component intrinsic profile.","marker":"Parent et al. 2022"}],"fun_headline_variants":["FAST scattering catalog: 149 pulsars, 113 first-time","Scattering timescales and spectral indices for 149 pulsars","FAST detects pulse broadening in 149 pulsars","First scattering measurements for 113 pulsars from FAST"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"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.","fun_headline_variants_meta":{"raw":{"variants":["FAST scattering catalog: 149 pulsars, 113 first-time","Scattering timescales and spectral indices for 149 pulsars","FAST detects pulse broadening in 149 pulsars","First scattering measurements for 113 pulsars from FAST"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000611,"raw_usage":{"total_tokens":2928,"prompt_tokens":1114,"completion_tokens":1814,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":730,"completion_tokens_details":{"reasoning_tokens":1744}},"tokens_in":730,"tokens_out":1814,"duration_ms":14271,"temperature":1.0,"reasoning_tokens":1744,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-07T00:18:47.238149+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"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.","supporting_citations":[],"review_version":1}