{"id":"e053e102-00e5-492f-af93-2975da705d3f","arxiv_id":"2605.14713","paper_version":1,"verdict":"UNVERDICTED","confidence":"LOW","novelty_score":4.0,"correctness_risk":"unknown","formal_verification":"none","parameter_count":0,"one_line_summary":"Asteroseismic characterisation of 32 bright stars in PLATO LOP fields using TESS data yields mode parameters for 26 stars extracted for the first time, with comparisons across three pipelines.","lead":"This paper extracts detailed asteroseismic parameters from TESS photometry for 32 bright naked-eye stars in the PLATO long-observation fields. These stars are positioned to serve as early test cases for calibrating the PLATO mission's oscillation analysis tools.","discovery_kind":"new_application","skeptic_critique":{"model":"grok-4.3","headline":"Mixed-mode inconsistencies in sub-giants flag that statistical pipeline selection may not yield reliable parameters for PLATO calibration","rationale":"The reader's weakest_assumption directly captures the abstract's own caveat on sub-giant mixed modes. No stronger internal inconsistency appears in the provided abstract text; the forward-looking claim about PLATO utility is tempered by this acknowledged limitation, supporting the existing UNVERDICTED verdict with low confidence. Full-text details on how many of the 32 are sub-giants or how the statistical criteria were applied would be needed to escalate the concern.","tokens_in":1854,"tokens_out":371,"duration_ms":13443,"concrete_test":"For the sub-giant stars among the 32, compare the mixed-mode frequencies and identifications from the three pipelines against each other and against any independent TESS re-analysis or ground-based spectroscopy; if the selected 'optimal' set still shows frequency differences >3 times the formal uncertainties or fails to match expected period spacing, the parameters cannot yet support reliable PLATO calibration without additional data.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central claim requires that the derived seismic parameters (large/small separations, asymptotic phase term, amplitudes, linewidths) from the 32 stars are sufficiently robust to serve as calibrators. The abstract explicitly states that 'in sub-giants, mixed-mode identification differs in the three pipelines, revealing extraction inconsistencies requiring longer datasets to improve our mode identifications.' This directly undercuts the assumption that applying statistical criteria across pipelines will identify an 'optimal' calibration/cadence/fitting combination, because the discrepancies indicate data-length limitations rather than resolvable methodological differences. For the subset of sub-giants (which are part of the 32), this creates a correctness risk for the parameters intended for PLATO validation.","agreement_with_reader":"agree"},"referee_report":{"model":"grok-4.3","summary":"The paper presents an asteroseismic characterisation of 32 bright (V<6) main-sequence and sub-giant stars from the TESS Luminaries sample that lie in the PLATO LOP fields. Using three independent pipelines (one similar to the official PLATO pipeline), the authors extract individual mode parameters for 26 stars for the first time, apply statistical criteria to select the optimal combination of data calibration, cadence and fitting method per star, and report large/small separations, asymptotic phase term, radial-mode amplitudes and mean linewidths per order. They note consistent trends across pipelines but flag that mixed-mode identification differs among pipelines for sub-giants, requiring longer datasets; they conclude that the sample will be crucial for validating, calibrating and optimising PLATO's seismic performance.","tokens_in":1987,"tokens_out":496,"duration_ms":21545,"significance":"If the extracted parameters are shown to be robust, the sample would constitute a valuable set of bright, naked-eye targets observable by PLATO from commissioning onward, enabling direct tests of the PLATO pipeline and early science operations. The use of a pipeline analogous to PLATO's is a positive feature for direct comparability.","major_comments":[{"comment":"Abstract: The assertion that 'comparisons reveal consistent trends in the seismic parameters, confirming the robustness of our analysis' is directly contradicted by the immediately following statement that 'in sub-giants, mixed-mode identification differs in the three pipelines, revealing extraction inconsistencies requiring longer datasets to improve our mode identifications.' Because sub-giants form part of the 32-star sample intended for PLATO calibration, this internal tension undermines the central claim that the derived parameters are sufficiently reliable for validating PLATO's seismic performance.","section":"Abstract"},{"comment":"Abstract: The manuscript provides no quantitative metrics (e.g., inter-pipeline differences in derived frequencies, amplitudes or linewidths, or the outcome of the statistical selection criteria) to support the claim of robustness, nor does it report error bars or exclusion rules for the final parameters. This absence is load-bearing for the PLATO-calibration conclusion.","section":"Abstract"}],"minor_comments":[{"comment":"Abstract: 'Statistical criterion were applied' should read 'Statistical criteria were applied'.","section":"Abstract"}],"recommendation":"major_revision","confidential_remarks":null},"author_rebuttal":{"model":"grok-4.3","summary":"We thank the referee for their careful and constructive review, which identifies key areas for improving the clarity of our abstract. We address the two major comments point by point below and will revise the abstract accordingly to strengthen the manuscript.","responses":[{"response":"We acknowledge that the abstract wording creates an apparent tension that could be misinterpreted. The phrase on consistent trends applies specifically to the global seismic parameters (large and small separations, asymptotic phase term, radial-mode amplitudes, and mean linewidths), which exhibit agreement across the three pipelines. The mixed-mode identification differences are isolated to sub-giants and are presented as a known limitation of current datasets rather than a refutation of overall robustness. The sample remains suitable for PLATO calibration on the basis of the robust global parameters. We will revise the abstract to explicitly separate these elements, qualify the robustness claim, and note the sub-giant caveat without implying contradiction.","revision_made":"yes","referee_comment":"[Abstract] Abstract: The assertion that 'comparisons reveal consistent trends in the seismic parameters, confirming the robustness of our analysis' is directly contradicted by the immediately following statement that 'in sub-giants, mixed-mode identification differs in the three pipelines, revealing extraction inconsistencies requiring longer datasets to improve our mode identifications.' Because sub-giants form part of the 32-star sample intended for PLATO calibration, this internal tension undermines the central claim that the derived parameters are sufficiently reliable for validating PLATO's seismic performance."},{"response":"We agree that the abstract would benefit from explicit quantitative support. The full manuscript applies statistical selection criteria per star and presents pipeline comparisons (including parameter tables) in the results sections, with error bars on individual frequencies. To address the referee's concern directly, we will add concise quantitative metrics to the abstract—such as typical inter-pipeline frequency differences and the fraction of stars with consistent selections—while referencing the error bars and exclusion rules already detailed in the text. This will better substantiate the PLATO-calibration utility.","revision_made":"yes","referee_comment":"[Abstract] Abstract: The manuscript provides no quantitative metrics (e.g., inter-pipeline differences in derived frequencies, amplitudes or linewidths, or the outcome of the statistical selection criteria) to support the claim of robustness, nor does it report error bars or exclusion rules for the final parameters. This absence is load-bearing for the PLATO-calibration conclusion."}],"tokens_in":1578,"tokens_out":516,"duration_ms":26256,"standing_objections":[]},"desk_editor":{"model":"grok-4.3","letter":"The main takeaway is that this work supplies individual mode parameters for 26 bright naked-eye stars in the PLATO LOP fields for the first time, using TESS data and three pipelines. That sample is genuinely useful because these stars will be visible to PLATO right away and can serve as early reference points.\n\nWhat the paper does is straightforward: it processes the TESS light curves through multiple independent codes, picks the best combination per star by a statistical rule, and reports large and small separations, asymptotic phase, amplitudes, and linewidths. For the main-sequence stars the trends line up across pipelines, which is the part that looks solid.\n\nThe soft spot is exactly what the abstract states about the sub-giants. Mixed-mode identification differs between the three pipelines, and the authors themselves say this points to extraction inconsistencies that need longer datasets. Sub-giants are part of the 32-star sample, so the claim that the whole set will validate and calibrate PLATO seismic performance rests on parameters that the paper itself marks as unreliable for that subset. Without quantitative error bars, exclusion criteria, or cross-checks against independent data in the abstract, it is hard to judge how large the problem is.\n\nThis paper is for teams already working on PLATO commissioning and early asteroseismic calibration. A reader who needs the specific targets and the pipeline comparison will get something concrete from it. The central argument does not collapse, but the sub-giant section needs tightening before the calibration use case is convincing.\n\nI would send it to peer review. The target list is timely and the multi-pipeline approach is worth documenting, even if the sub-giant results require more work or caveats.","headline":"The paper gives first seismic parameters for 26 of 32 bright PLATO-field stars but the sub-giant mixed-mode discrepancies flagged in the abstract limit how far the calibration claim can be trusted.","tokens_in":2547,"tokens_out":426,"would_cite":false,"duration_ms":13939,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"grok-4.3","headline":"The 32 naked-eye stars in the PLATO long-duration fields form a ready calibration set for the mission's asteroseismology.","keywords":["asteroseismology","solar-like oscillations","TESS mission","PLATO mission","bright stars","seismic parameters","mode identification"],"falsifier":"Future PLATO observations of these same stars yielding mode parameters or frequency separations that differ substantially from the TESS-derived values.","tokens_in":2768,"feed_emoji":"🔭","tokens_out":605,"duration_ms":29854,"temperature":0.7,"pith_summary":"The paper provides detailed asteroseismic analysis of 32 bright stars that lie in the fields PLATO will observe for long periods. Using TESS photometry and three different analysis pipelines, the authors extract oscillation mode parameters for most of these stars and select the best data processing approach for each. If correct, this positions the sample as an immediate resource for testing and refining PLATO's seismic measurements from the mission's start. Readers would care because these nearby stars offer a direct way to check how well the new observatory captures solar-like oscillations.","feed_headline":"32 naked-eye stars prepared as PLATO seismic calibrators","feed_subtitle":"TESS analysis of stars in the mission's long fields yields mode parameters and optimal pipelines for early validation.","key_machinery":"The set of 32 Luminaries stars in the PLATO LOP fields, processed through three independent seismic pipelines to determine optimal analysis settings and extract mode parameters.","core_discovery":"Individual mode parameters were extracted for the first time for 26 of the 32 stars. Statistical criteria were used to choose the optimal combination of data calibration, cadence, and fitting method for each star. Derived quantities include large and small separations, asymptotic phase term, radial mode amplitudes, and mean linewidths. The analysis confirms consistent trends across pipelines while noting inconsistencies in mixed-mode identification for sub-giants.","pith_inferences":["Future work could test whether the selected pipeline combinations remain optimal when applied to actual PLATO observations.","Similar multi-pipeline approaches might improve characterization of other bright oscillating stars outside these fields.","The inconsistencies noted suggest that mode identification accuracy depends strongly on observation length for evolved stars."],"forward_implications":["These stars can serve as early calibrators during PLATO commissioning and initial operations.","Longer datasets will be needed to resolve mixed-mode identification issues in sub-giants.","Derived seismic parameters such as separations and amplitudes show robustness across different pipelines.","The sample enables direct comparison of TESS-based results with upcoming PLATO data."],"fun_headline_variants":["First modes extracted for 26 naked-eye PLATO stars","Optimal combos of data and pipelines for 32 stars","Large and small separations for naked-eye stars","Mixed-mode differences in three pipeline outputs"],"cache_read_input_tokens":2112,"weakest_assumption_plain":"The statistical criteria applied to results from the three pipelines can reliably identify the optimal data calibration, cadence, and fitting method for each star.","fun_headline_variants_meta":{"raw":{"variants":["First modes extracted for 26 naked-eye PLATO stars","Optimal combos of data and pipelines for 32 stars","Large and small separations for naked-eye stars","Mixed-mode differences in three pipeline outputs"]},"model":"grok-4.3","cost_usd":0.00689,"raw_usage":{"total_tokens":3179,"prompt_tokens":792,"num_sources_used":0,"completion_tokens":57,"cost_in_usd_ticks":68903000,"prompt_tokens_details":{"text_tokens":792,"audio_tokens":0,"image_tokens":0,"cached_tokens":64},"completion_tokens_details":{"audio_tokens":0,"reasoning_tokens":2330,"accepted_prediction_tokens":0,"rejected_prediction_tokens":0}},"tokens_in":792,"tokens_out":57,"duration_ms":9889,"temperature":1.0,"reasoning_tokens":2330,"cache_read_input_tokens":64,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-06-30T20:24:59.822304+00:00","model_set":{"reader":"grok-4.3"},"falsifier":"Future PLATO observations of these same stars yielding mode parameters or frequency separations that differ substantially from the TESS-derived values.","supporting_citations":[],"review_version":1}