{"id":"7a213a57-e7c2-41c3-bbf1-825aef09edfe","arxiv_id":"2602.14294","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":5,"one_line_summary":"A four-stage quantitative filter applied to CRIRES spectra of six Gaia benchmark stars yields per-stellar-type robust atomic line lists in the Y, J, and H bands, anchored to laboratory data.","lead":"This paper tests thousands of near-infrared absorption lines against high-resolution spectra of six benchmark stars and keeps only those that pass four quantitative filters: depth, non-saturation, purity, and fit quality. The result is a laboratory-anchored line list for the Y, J, and H bands plus a reproducible pipeline for extending it.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The published robust lists are internally inconsistent: Appendix A and Table B.1 disagree by large factors (M-giant H: 8 Fe I/5 Si I vs 0/1; G-dwarf H: 16 Fe I vs 4), so the central data product is not reproducible as printed.","rationale":"I read the paper as aiming to deliver a quantitative, laboratory-anchored infrared line list, and I agree with the reader that the framework is plausible in outline: the thresholds are disclosed, the input parameters are externally anchored, and the external overlaps with APOGEE, Şentürk et al., and Marfil et al. provide some independent support. However, the single most load-bearing problem I found is not the LTE assumption, which the authors acknowledge and quantify, but an internal contradiction in the delivered product. Table B.1 is explicitly presented as the summary of the final YYYY lists, yet it disagrees with Appendices A.1–A.6 by large factors and even by species presence. The reader's conditional verdict is therefore justified, but for a more immediate, checkable reason than the one named in the weakest_assumption: the paper's own tables do not define a unique robust line list. I do not see this as an ad hominem or a philosophical objection; it is a data-integrity issue that can be settled by counting lines and re-running the pipeline. Until the authors reconcile Appendix A with Table B.1—or make the pipeline output available so users can regenerate the counts—the central product cannot be adopted unambiguously.","tokens_in":25071,"tokens_out":11180,"duration_ms":98408,"concrete_test":"Parse Appendices A.1–A.6 and count entries per species, band, and stellar class; compare against Table B.1. At minimum verify (a) H-band M giant: Appendix A.6 has 18 lines while Table B.1 sums to 5; (b) H-band G dwarf: A.2 has 40 lines while B.1 sums to 35–36. Then rerun the published selection code on the same VALD3/MARCS inputs to determine which table reflects the actual YYYY outcomes. If Appendix A is correct, Table B.1 must be regenerated; if Table B.1 is correct, the Appendix A lists contain non-YYYY entries and the robust list as printed is invalid.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Appendix B states that Table B.1 reports \"the number of transitions that pass all selection criteria\" per class, i.e., the final YYYY outcomes. Its numbers must therefore match the contents of Appendices A.1–A.6. They do not. Example: H-band M giant. Appendix A.6 lists 18 robust lines: 8 Fe I (16008.075, 16039.853, 16040.654, 16072.242, 16231.646, 16316.320, 16486.666, 16753.065), 4 Mg I, 5 Si I, and V I 15774.060. Table B.1's H-band M-giant column sums to 5 (Mg I=4, Si I=1), gives Fe I=0, and has no V I row. Similar mismatches occur for the G-dwarf H band (A.2 lists 16 Fe I, 9 Si I, and K I 15168.376; B.1 lists 4, 16, and 0), the F-dwarf H band (A.1 has 4 Si I; B.1 has 6), and the J-band M giant (A.6 has 7 Fe I, 10 Si I, 3 Cr I, 7 Ti I; B.1 has 4, 8, 0, 5). These are not cosmetic typos in one wavelength value; the two published summaries of the central deliverable contradict each other. A user cannot tell which lines are actually recommended, so the central claim—a reproducible YYYY robust list—is not currently supported by the manuscript as printed.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper presents a quantitative, multi-criteria pipeline for selecting robust atomic absorption lines in the near-infrared Y, J, and H bands (9800–18000 Å) for abundance analyses of FGK stars. Six Gaia FGK Benchmark Stars observed with CRIRES+ are analyzed using 1D-LTE MARCS/MOOG synthetic spectra computed from VALD3 laboratory atomic data and benchmark stellar parameters. Each candidate transition is evaluated for line depth, saturation, purity (blending), and goodness of fit against observed profiles. Lines that pass all four criteria in a given band are labeled YYYY and compiled as 'robust' lists per spectral type in Appendices A.1–A.6, with input–output counts summarized in Table B.1. The robust lists are cross-matched against APOGEE, Şentürk et al. (2024), and Marfil et al. (2020), showing partial overlap. The paper claims to provide a reproducible, laboratory-grounded line list useful across a wide range of stellar parameters.","tokens_in":25357,"tokens_out":6798,"duration_ms":64648,"significance":"If the reported lists were internally consistent, the paper would offer a valuable community resource: a homogeneous NIR line selection based on a transparent, deterministic decision tree, with genuinely external validation through cross-matching (33 transitions in common with APOGEE for the Sun, 24 for Arcturus, 22 with Şentürk, and 15 Fe I with Marfil). The pipeline is described in sufficient detail to be rerun as atomic data improve, and the authors explicitly recognize several modeling limitations (LTE-only synthesis, missing molecular data for the coolest star, approximate abundance scaling). However, the central data product is compromised as printed: the robust line lists in Appendices A.1–A.6 and the summary counts in Table B.1 contradict each other by large factors for many spectral classes and bands. A user cannot determine which transitions are actually recommended. In addition, the GoF step tests consistency with abundance assumptions that are not independently constrained for alpha-elements in metal-poor stars. These issues are load-bearing for the paper's main claim, though they appear fixable by re-running the pipeline and performing targeted sensitivity tests.","major_comments":[{"comment":"The manuscript states that Table B.1 reports 'the number of transitions that pass all selection criteria' (i.e., final YYYY outcomes), so its numbers must match the contents of Appendices A.1–A.6. They do not. For example, H-band M giant: Appendix A.6 lists 8 Fe I, 5 Si I, and 1 V I, while Table B.1 gives Fe I=0, Si I=1, and no V I row. G-dwarf H: Appendix A.2 lists 16 Fe I and 9 Si I, but Table B.1 gives Fe I=4 and Si I=16. F-dwarf H: Appendix A.1 lists 4 Si I, but Table B.1 gives 6. J-band M giant: Appendix A.6 lists 7 Fe I, 10 Si I, 3 Cr I, and 7 Ti I, but Table B.1 gives 4, 8, 0, and 5. These are not minor typos in a wavelength entry; the two published summaries of the central deliverable are systematically inconsistent. As printed, the robust list is not reproducible, and the main claim is unsupported. The authors must reconcile these tables, explain the discrepancy (e.g., counting","section":"Appendix A vs Appendix B, Table B.1"},{"comment":"The GoF stage evaluates how well a synthesis matches the observed spectrum, but the synthesis uses [X/H] scaled to the star's global [M/H] for elements without individual optical abundances, including Si. For Arcturus ([Fe/H]=−0.55, [α/Fe]∼+0.3), this sets [Si/H]≈−0.55 instead of the likely ≈−0.25. The synthetic Si lines are then too weak, and the GoF may reject a perfectly good Si line because the input abundance is wrong, or accept a line only because the abundance error compensates for atomic-data error. Since the paper's cross-match counts and robust lists emphasize Si I lines, this assumption is load-bearing for the alpha-element conclusions. Please run a sensitivity test: redo the Si I selection for Arcturus with [Si/H] from the literature (or with [Si/Fe]=+0.3) and report whether the YYYY decisions change. If they do, the claim of robustness across the full stellar-parameter range","section":"Sections 3.1 and 3.2.4, Table 2"},{"comment":"The depth threshold is d≥0.03, and the paper states that for S/N∼100, Eq. (1) gives σ≈0.01, so d=0.03 is a ∼3σ detection. However, the H-band spectrum of γ Sge has S/N=37.8 (Table 1), for which σ=1/37.8≈0.026 and d=0.03 is only a ∼1.2σ feature. The M-giant H-band robust list (Appendix A.6) is therefore potentially dominated by noise fluctuations. The selection should either mask this low-S/N band/class, apply an S/N-dependent depth threshold, or provide a quantitative justification for why the fixed 0.03 threshold remains reliable at S/N≈38. Without this, the H-band M-giant conclusions are not supported.","section":"Section 3.2.1, Eq. (1), Table 1"},{"comment":"The entire selection is based on 1D-LTE synthesis, while the paper itself cites NLTE abundance corrections up to 0.2 dex for IR lines of Si I and Ca II (Section 3.2.1). A line that passes the GoF in LTE may fail when NLTE effects are included, and vice versa. Although the authors frame this as a framework that can be updated, the central claim is that the selected lines are 'robust' for abundance work. The paper should quantify how many of the final YYYY lines have known NLTE corrections exceeding, say, 0.1 dex, and whether any of the rejected lines would be recovered under NLTE. This is a concrete, testable addition that would materially strengthen the robustness claim.","section":"Sections 3.1 and 3.2.1"}],"minor_comments":[{"comment":"The cross-match paragraph states 33 transitions in common with APOGEE for the G dwarf, but the breakdown (12 Fe I + 9 Si I + 4 Mg I + 3 N I + 3 C I + 1 Si + 1 Cr I + 1 K I) sums to 34. Please check the count.","section":"Section 4"},{"comment":"In the text describing saturation, 'a line is flagged as Unsaturated N when...' should presumably read 'flagged as saturated' (the N flag indicates saturation). The placeholder 'element_id' in the same section is unresolved.","section":"Section 3.2.2"},{"comment":"In the G-dwarf H-band list, 'Si15400.077' appears adjacent to 'Sii...' lines; please clarify whether this is Si I (neutral) or a separate species, and ensure consistent notation throughout the appendices.","section":"Appendix A.2, H band"},{"comment":"The nominal resolution is reported as 'R∼90000' in the introduction and '∼100000' in Section 2; Table 2 and the synthesis use R=90000. Please harmonize the values or explain the difference.","section":"Section 2"}],"recommendation":"major_revision","confidential_remarks":"The Appendix A vs Table B.1 discrepancy is severe enough that I would not consider acceptance until it is resolved. The good news is that the rest of the pipeline is transparent, so the fix should be possible by rerunning the counting step and checking the code. If the authors cannot produce a consistent table, the paper should not be published as a source of recommended lines. I also encourage the editor to ask for the sensitivity test on Si abundance for Arcturus; it directly affects the credibility of the alpha-element part of the lists."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Read this one if you care about infrared abundance work—the framework is actually well thought out, but the paper as printed has a load-bearing internal inconsistency that has to be resolved before anyone should use the lists. Appendix A (the robust YYYY lines per spectral type) and Table B.1 (which the text says reports the same final counts) disagree by large factors. Example: H-band M giant—Appendix A.6 lists 8 Fe I and 5 Si I; Table B.1 says 0 Fe I and 1 Si I. G-dwarf H: Appendix A.2 gives 16 Fe I and 9 Si I; B.1 gives 4 and 16. F-dwarf H: A.1 has 4 Si I; B.1 has 6. J-band M giant: A.6 has 7 Fe I, 10 Si I, 3 Cr I, 7 Ti I; B.1 has 4, 8, 0, 5. These aren't typographical slips; the two published summaries of the central deliverable contradict each other. A user cannot tell which lines are actually recommended.\n\nWhat's genuinely good: the four-stage flagging scheme (depth, saturation, purity, GoF) is transparent, deterministic, and the thresholds are mostly justified from S/N and telluric-residual floors. The cross-validation against APOGEE, Senturk et al., and Marfil et al. is a real strength, and the use of benchmark stars with interferometric/astrometric parameters avoids the usual circular fitting. The Y-band example lines (Si I and Sr II) are nicely walked through.\n\nThe other soft spots are smaller but worth naming. The synthesis is 1D-LTE while the paper itself cites up to 0.2 dex NLTE corrections for Si I and Ca II in the IR; with [Si/H] scaled from [M/H] for several stars, the purity and GoF flags are testing model consistency, not independently known abundances. There's also no end-to-end abundance recovery test, so \"robust\" means filter-stable, not abundance-accurate. And the per-band GoF threshold relaxation in J/H is post-hoc, though at least disclosed.\n\nBottom line: the methodology deserves referee time, and with the appendix counts reconciled this would be a useful community artifact. As printed, the central data product is not reproducible. I'd send it back for major revision on that basis.","headline":"Good method, broken table: the printed line lists contradict the summary counts, so the central data product isn't usable until fixed.","tokens_in":26076,"tokens_out":3653,"would_cite":false,"duration_ms":31077,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"This paper claims to deliver a laboratory-grounded, uniformly validated set of near-infrared atomic lines (Y, J, H bands) for stellar abundance determinations, selected by a quantitative four-stage filter applied to six benchmark stars span","keywords":["infrared spectroscopy","stellar abundances","line selection","atomic data","benchmark stars","spectral synthesis","line blending","goodness of fit"],"falsifier":"Take a star not in the sample (or one with independently known elemental abundances) and measure abundances from the paper's robust lines in two different bands; if the results disagree by more than the internal scatter, or if a line accepted as robust gives an abundance offset larger than the stated NLTE corrections (about 0.2 dex) when compared against an independent reference, the claim of cross-band and cross-stellar robustness is refuted.","tokens_in":24838,"feed_emoji":"🔭","tokens_out":4332,"duration_ms":40730,"temperature":0.7,"pith_summary":"The paper aims to solve a practical problem: infrared abundance measurements are less reliable than optical ones because line lists and models are less well validated. It proposes a reproducible, purely quantitative selection pipeline that takes atomic transitions in the Y, J, and H bands, tests each against depth, saturation, blending, and spectral-fit criteria, and keeps only lines that pass in all six benchmark stars. The result is a line list anchored to laboratory data rather than empirical calibration, with accepted lines dominated by Mg I, Si I, Ca I, and Fe I, plus Sr II as the only neutron-capture species. A sympathetic reader would care because this provides a community-usable reference and a template for re-validation as atomic data and instruments improve.","feed_headline":"Six benchmark stars filter a robust infrared line list","feed_subtitle":"A four-step quantitative test picks lines that stay reliable from F dwarfs to M giants.","key_machinery":"The key mechanism is a four-stage flagging decision tree. Each candidate transition is evaluated for depth (minimum central absorption 0.03), saturation (local curve-of-growth slope below 0.5 plus negligible core-flux change flags the line), purity (P = equivalent width in a 30 km/s window divided by that in a 60 km/s window; P>=0.75 accepted, 0.5–0.75 flagged undecided, <0.5 rejected), and goodness of fit (reduced chi-square, RMSE, and MAD against observed spectra, with relaxed thresholds in J and H bands to account for telluric residuals). Only lines that earn 'YYYY' in all four stages are included in the robust list.","core_discovery":"The central claim is that a set of atomic transitions in the near-infrared can be identified that behave consistently across a wide range of stellar parameters, so that they can be used for abundance determinations without object-dependent fine-tuning. The paper demonstrates this by applying a sequence of quantitative filters—line depth >=0.03, non-saturation via curve-of-growth slope and core-flux response, purity measured as the ratio of equivalent widths in two velocity windows, and goodness-of-fit statistics with band-specific thresholds—to synthetic spectra computed for six benchmark stars. The accepted lines are tabulated per spectral type in the appendices. The method is designed to b","pith_inferences":["Applying the same four-stage filter to other spectral bands (e.g., K or L bands) or to a larger sample of benchmark stars could extend the validated line library and test the thresholds' generality.","The purity criterion could be combined with 3D and NLTE synthetic spectra, since the paper itself notes IR NLTE corrections up to 0.2 dex; such tests might revise which lines survive.","The reproducibility of the pipeline means a community-driven effort could maintain a living line list, updating flags whenever atomic data are revised.","For elements lacking optical abundances, the practice of scaling to metallicity is a clear limitation; a dedicated star with independently determined abundances for those elements would make a sharper test."],"forward_implications":["NIR abundance analyses can adopt the tabulated lines as a library of reliable diagnostics across spectral types from F dwarfs to M giants.","The quantitative framework can be re-executed automatically as new laboratory atomic data, atmosphere models, or instruments become available.","The approach provides a way to detect problematic lines without empirical recalibration, isolating the atomic data or model as the source of disagreement.","The result that only Sr II among n-capture elements passes the tests implies that systematic searches for heavier-element lines in the NIR need further work.","The line list can serve as a cross-check for survey pipelines that rely on astrophysically calibrated lists."],"fun_headline_variants":["Six benchmark stars vet infrared lines for abundances","Robust IR lines identified via six-star quantitative test","Infrared line list proven stable across six benchmark stars","Reliable near-IR lines for abundances from six-star analysis","Quantitative screening yields consistent IR atomic lines"],"cache_read_input_tokens":2304,"weakest_assumption_plain":"The entire selection rests on the assumption that the 1D-LTE synthetic spectra computed with benchmark parameters and scaled abundances are accurate enough that a line's failure to match the observed profile is due to the line itself, not to the model or assumed abundance.","fun_headline_variants_meta":{"raw":{"variants":["Six benchmark stars vet infrared lines for abundances","Robust IR lines identified via six-star quantitative test","Infrared line list proven stable across six benchmark stars","Reliable near-IR lines for abundances from six-star analysis","Quantitative screening yields consistent IR atomic lines"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000206,"raw_usage":{"total_tokens":1254,"prompt_tokens":785,"completion_tokens":469,"prompt_tokens_details":{"cached_tokens":256},"prompt_cache_hit_tokens":256,"prompt_cache_miss_tokens":529,"completion_tokens_details":{"reasoning_tokens":396}},"tokens_in":529,"tokens_out":469,"duration_ms":4768,"temperature":1.0,"reasoning_tokens":396,"cache_read_input_tokens":256,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-02T23:15:27.299739+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Take a star not in the sample (or one with independently known elemental abundances) and measure abundances from the paper's robust lines in two different bands; if the results disagree by more than the internal scatter, or if a line accepted as robust gives an abundance offset larger than the stated NLTE corrections (about 0.2 dex) when compared against an independent reference, the claim of cross-band and cross-stellar robustness is refuted.","supporting_citations":[],"review_version":1}