{"id":"4be15f38-4f4c-483d-b900-375421ace047","arxiv_id":"2508.05734","paper_version":1,"verdict":"UNVERDICTED","confidence":"LOW","novelty_score":6.0,"correctness_risk":"unknown","formal_verification":"none","parameter_count":3,"one_line_summary":"Short-period sub-Neptunes peak at about 3750 K around early-type M dwarfs, matching pebble accretion predictions, while super-Earths keep rising toward cooler stars.","lead":"This paper analyzes Kepler and K2 data to measure how often short-period, Earth- to Neptune-sized planets orbit stars from 3200 K to 6900 K. It finds that sub-Neptunes peak around early M dwarfs near 3750 K, as pebble accretion models predicted, while super-Earths keep rising toward cooler stars.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"Unverifiable central claim: the submitted full text is an unrelated cosmology paper, so the 3750 K sub-Neptune peak has no supporting methods, sample, or corrections in evidence.","rationale":"The reader's verdict is UNVERDICTED, and my read keeps that. The load-bearing issue is more fundamental than the reader's weakest_assumption: the submitted full text is a different paper, so the occurrence-rate analysis itself is missing. The reader instead identifies the completeness/Teff bias as the key scientific assumption—which is exactly the right soft spot if the real methods were present. I therefore partially agree: the reader names the science-level risk, but the immediate blocker is the total absence of the supporting document, not a specific bias within it. The concrete test first resolves the document mismatch and, in the branch where the real paper exists, tests the completeness/Teff sensitivity that would decide whether the peak is real. This supports an UNVERDICTED disposition rather than ACCEPT or REJECT: absence of evidence is not evidence of a false peak, but the central claim cannot be checked from this submission.","tokens_in":8852,"tokens_out":7775,"duration_ms":79638,"concrete_test":"Query the arXiv API for record 2508.05734 and compare the official title and abstract with the submitted abstract. If the official record is the cosmology paper (matching the supplied full text), the exoplanet occurrence-rate analysis is not present and the 3750 K peak is unsupported. If the official record instead matches the K2 abstract, retrieve the actual PDF and check that the methods section contains the completeness model and Teff calibration; then independently rerun the occurrence-rate calculation on the public Kepler DR25/K2 DR2 catalogs using the same 130-planet cuts and at least two M-dwarf Teff scales, and verify whether the peak shifts by more than the quoted +153/-97 K uncertainties.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The abstract's central claim is a uniform Kepler+K2 occurrence-rate analysis: 130 short-period sub-Neptunes, a peak at 3750 K, and a first observational confirmation of pebble-accretion predictions. The supplied full text, however, is an entirely different manuscript—'Detecting Model Misspecification in Cosmology with Scale-Dependent Normalizing Flows' (Akhmetzhanova et al.)—containing no mention of Kepler, K2, M dwarfs, transits, completeness, or effective temperatures. Every load-bearing component of the claim is therefore absent: the planet candidate sample, the detection-completeness model in period-radius-TeFF space, the treatment of K2 GO target selection, the adopted Teff scale, and the occurrence-rate estimator with uncertainties. This matters because the claimed shape (sub-Neptunes peaking at early-M, super-Earths rising) is exactly what completeness and Teff corrections can distort: cooler M dwarfs yield smaller transit depths at fixed radius, and K2's guest-observer M-dwarf sample is not selected like Kepler's. If the completeness model or temperature scale varies with spectral type differently than assumed, a 3750 K peak could be an artifact. The document as received is internally inconsistent; per review policy this is not dismissed as a pipeline artifact. This is an absence-of-evidence problem—it does not prove the astrophysical result false, but it makes the central claim unverifiable as submitted.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"The submission consists of an abstract reporting a uniform Kepler+K2 occurrence-rate study of short-period ($P=1-40$ d) Earth- to Neptune-sized planets around M dwarfs, claiming a sub-Neptune occurrence peak at $3750^{+153}_{-97}\\,\\mathrm{K}$, declining occurrence toward cooler M dwarfs, and a first observational confirmation of pebble-accretion model predictions. The full text supplied with the manuscript, however, is an unrelated cosmology paper, 'Detecting Model Misspecification in Cosmology with Scale-Dependent Normalizing Flows' (Akhmetzhanova et al.), with no mention of Kepler, K2, M dwarfs, transits, occurrence rates, completeness corrections, or stellar temperatures. Consequently, none of the methods, sample definitions, completeness models, temperature-scale choices, or comparison calculations needed to support the abstract's claims are present in the submitted document.","tokens_in":9165,"tokens_out":2710,"duration_ms":29895,"significance":"The headline astrophysical result—if correct—would be significant: it would change the picture of small-planet formation around M dwarfs from a monotonic increase toward cooler stars to a peaked distribution near early-M temperatures, providing a direct test of pebble-accretion models. The paper, as submitted, provides no verifiable evidence for this result. There are no machine-checked proofs, reproducible code, or parameter-free derivations in the supplied body text; the only quantitative content is the abstract. The claimed peak location and the confirmation of theoretical predictions therefore cannot be independently assessed. Because the supplied full text is a different paper, the manuscript in its current form does not meet the standard of a publishable research article.","major_comments":[{"comment":"The body of the manuscript is an unrelated cosmology paper: it develops scale-dependent normalizing flows for detecting model misspecification in CAMELS simulations. It contains no mention of Kepler, K2, M dwarfs, transit photometry, or planet occurrence. Every load-bearing element of the abstract—the 130-planet sample, the period/radius/T_eff cuts, the occurrence-rate estimator, and the quoted uncertainties on the 3750 K peak—is therefore absent. This is not a stylistic defect but a complete absence of the central derivation. The central claim cannot be verified or falsified from the submitted text.","section":"Full text (all sections)"},{"comment":"The abstract states that Kepler and K2 data were 'uniformly combined,' but no detection-completeness model in period-radius-T_eff space is presented. Without such a model, the reported peak could reflect the varying sensitivity of K2's guest-observer target selection and the smaller transit depths of cooler M dwarfs at fixed planet radius. The text provides no way to check whether the 3750 K peak is an astrophysical feature or an artifact of completeness corrections.","section":"Abstract; Section 2 (missing completeness model)"},{"comment":"The peak temperature depends directly on the adopted effective-temperature scale and binning for M dwarfs, as well as on the radius boundaries used to separate sub-Neptunes from super-Earths. None of these are defined. The abstract gives only the peak value and uncertainties; without the binning scheme, the boundary definitions, and the temperature scale, the claim that occurrence peaks at early-M temperatures is not reproducible.","section":"Abstract; Section 3 (missing T_eff scale and binning)"},{"comment":"The abstract claims that a peak 'near this location was predicted by pebble accretion planet formation models and confirmed here by observations for the first time.' The manuscript provides no specific predictions, no citations to the models, no quantitative comparison metric, and no discussion of whether the model predictions were made independently of the Kepler/K2 data. The confirmation claim is therefore unsupported. This is a load-bearing part of the paper's contribution and cannot be evaluated from the submitted text.","section":"Abstract (pebble-accretion comparison)"}],"minor_comments":[{"comment":"The manuscript header displays the arXiv identifier 2508.05744 and an author list that match the cosmology paper, while the submission ID is 2508.05734 and the abstract is an exoplanet-occurrence paper. This internal inconsistency is consistent with a manuscript assembly error and should be corrected if a corrected submission is provided.","section":"Header/Abstract"},{"comment":"Because the body text is unrelated to the abstract, no assessment of figures, tables, or presentation quality of the occurrence-rate analysis is possible. A corrected submission would need to include the full methods, sample definition, completeness treatment, and theory comparison before standard refereeing can proceed.","section":"General"}],"recommendation":"reject","confidential_remarks":"The submitted file contains an abstract from one paper and the full text of a different paper. This is not a case of a minor technical flaw; the entire evidential basis of the reported result is missing. Even though the astrophysical claim may be plausible and important, the manuscript as submitted cannot be meaningfully reviewed. I recommend rejection, with the possibility that the authors resubmit a correct, complete manuscript as a new submission. This decision should not be taken as a negative judgment on the underlying scientific claim, which may be sound."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"First: the abstract is exactly the kind of result that matters—a uniform Kepler+K2 occurrence rate across FGK and M dwarfs, with sub-Neptunes peaking at 3750 K and super-Earths still climbing. If the underlying analysis holds, that's the first observational anchor for pebble-accretion predictions around early-M dwarfs, and it would directly shape TESS/Roman/PLATO target lists. Credit where due: the abstract lays out a sensible design and a falsifiable claim.\n\nHere's the problem: the full text I was sent is not this paper. It's a cosmology manuscript on normalizing flows and model misspecification. There is no Kepler, no K2, no completeness model, no Teff scale, no occurrence estimator. Absolutely nothing in the body supports the abstract. This is not a missing methods section. Every load-bearing component—the 130-planet sample, the detection-completeness corrections in period-radius-Teff space, the treatment of K2 guest-observer selection, the adopted temperature scale, the false-positive handling—is absent. The reader's stress test is right: a 3750 K peak could be an artifact of where completeness or the Teff scale changes, and we have no way to check.\n\nTo be clear, this is an absence-of-evidence problem, not evidence against the result. The abstract could be right. I'm also not assuming the authors did anything wrong; this could be a submission mix-up. But taking the manuscript as it stands, it is internally inconsistent, and the central claim is unverifiable. The confirmation claim about pebble accretion also can't be audited—we can't tell whether the prediction predates the data or how independent it is.\n\nWhat's softest is not the astrophysics; it's the submission. I can't recommend sending this document to a referee. The right move is to desk-return it and ask the authors to submit the correct paper. If the real manuscript matches the abstract, then yes, it deserves a serious referee—the question it answers is important and the field would value it. But as received, there is nothing to review.\n\nBottom line: this is a paper worth reading when it actually exists. Right now it doesn't.","headline":"The abstract promises an important result; the submitted body is a different paper, so the claim is unverifiable as received.","tokens_in":9708,"tokens_out":3039,"would_cite":false,"duration_ms":28078,"reading_group":"no","serious_thinker":"no","would_accept_peer_review":false},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"Short-period sub-Neptunes around M dwarfs are most common near 3750 K and decline for cooler stars.","keywords":["exoplanet occurrence rates","M dwarfs","sub-Neptunes","super-Earths","Kepler","K2","pebble accretion","transit surveys"],"falsifier":"Re-derive the occurrence rates from the same candidate list using an independent M dwarf temperature scale, such as bolometric fluxes or interferometric radii, and a separate completeness model, then check whether the turnover at 3750 K persists; if it shifts below roughly 3500 K or disappears, the claimed peak is not robust. The claim would also be weakened if a future uniformly selected transit survey of mid-to-late M dwarfs finds sub-Neptune occurrence staying flat or rising.","tokens_in":8759,"feed_emoji":"🪐","tokens_out":7776,"duration_ms":73394,"temperature":0.7,"pith_summary":"This paper tries to establish that short-period (1-40 day) sub-Neptune planets around M dwarfs are not uniformly common: their occurrence rate rises toward early M stars, peaks near an effective temperature of 3750 K, and falls for cooler M dwarfs. The authors reach this by merging Kepler and K2 transit surveys into one catalog of 130 Earth-to-Neptune-sized planet candidates around M dwarfs, with K2 contributing nine times more M dwarf targets than Kepler. If true, it is the first observational confirmation of a peak near the location predicted by pebble accretion formation models, and it shows that small-planet occurrence around the lowest-mass stars is not a simple monotonic increase. Super-Earths, by contrast, continue to increase in occurrence toward cooler stars, with no clear peak in the 3200-6900 K range.","feed_headline":"Sub-Neptunes around M dwarfs peak at 3750 K","feed_subtitle":"A combined Kepler-K2 count of 130 small planets finds sub-Neptunes fade for cool stars while super-Earths keep rising.","key_machinery":"The central object is the occurrence-rate calculation built from a uniform combination of Kepler and K2 transit catalogs, yielding 130 short-period ($P=1$-$40$ days) Earth-to-Neptune-sized candidates around M dwarfs. The load-bearing comparison is the distribution of these rates as a function of host-star effective temperature against the pebble accretion model prediction of a peak near early-M temperatures. The K2 sample's much larger M dwarf census supplies the statistical power at the cool end where Kepler had few targets.","core_discovery":"The paper claims that after uniformly combining Kepler and K2 data and correcting for completeness, short-period sub-Neptune occurrence peaks at $3750^{+153}_{-97}\\,\\mathrm{K}$ and declines for cooler host stars. K2, whose targets were chosen by guest observers, observed nine times more M dwarfs than Kepler and 3.5 times more of these small planets around hosts below 3700 K. The observed peak is reported as the first confirmation of a feature near that temperature predicted by pebble accretion models. In the same host-star range, super-Earth occurrence keeps rising toward cooler M dwarfs without a detected turnover.","pith_inferences":["The text after the abstract is a different manuscript, so this summary rests on the abstract alone; the completeness and temperature-scale methods behind the peak still need to be inspected in the actual occurrence-rate paper.","If the turnover is physical, occurrence-rate templates used to predict yields for future missions should not extrapolate the early-M rise to later M dwarfs, or they will overpredict cool-host sub-Neptunes.","A testable consequence is that precise radii and temperatures for a large mid-to-late M dwarf sample should show the sub-Neptune-to-super-Earth ratio decreasing monotonically below roughly 3500 K, if the paper's reading of the data is correct.","Because K2's targets were selected by guest observers, an independent, uniformly selected M dwarf transit survey would provide the cleanest check of whether the completeness corrections, rather than astrophysics, create the peak."],"forward_implications":["If the 3750 K peak is real, planet formation around M dwarfs is not a monotonic function of stellar mass: sub-Neptune formation becomes less efficient for the coolest, lowest-mass stars.","Pebble accretion models that predicted a peak near this temperature gain a quantitative observational target; refining them now requires matching both the peak location and its width.","Super-Earths and sub-Neptunes must have formation paths that respond differently to host-star temperature, since one population turns over while the other does not.","Future transit surveys of mid-to-late M dwarfs should test the predicted decline by adding many more cool-host planets.","The combined Kepler and K2 M dwarf sample, rather than either survey alone, is what makes the cool end measurable."],"supporting_citations":[],"fun_headline_variants":["M dwarf sub-Neptunes peak at 3750 K","Sub-Neptune occurrence peaks at 3750 K for M dwarfs","Kepler-K2 pinpoints sub-Neptune peak around 3750 K","Super-Earths rise while sub-Neptunes peak at 3750 K","Short-period sub-Neptunes max out near 3750 K"],"cache_read_input_tokens":2816,"weakest_assumption_plain":"The result stands on the assumptions about how many planets the Kepler and K2 surveys missed around each star and on the temperatures assigned to M dwarfs; if either is biased by spectral type, the peak at 3750 K could be an artifact rather than a real feature.","fun_headline_variants_meta":{"raw":{"variants":["M dwarf sub-Neptunes peak at 3750 K","Sub-Neptune occurrence peaks at 3750 K for M dwarfs","Kepler-K2 pinpoints sub-Neptune peak around 3750 K","Super-Earths rise while sub-Neptunes peak at 3750 K","Short-period sub-Neptunes max out near 3750 K"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000199,"raw_usage":{"total_tokens":1212,"prompt_tokens":751,"completion_tokens":461,"prompt_tokens_details":{"cached_tokens":256},"prompt_cache_hit_tokens":256,"prompt_cache_miss_tokens":495,"completion_tokens_details":{"reasoning_tokens":377}},"tokens_in":495,"tokens_out":461,"duration_ms":4973,"temperature":1.0,"reasoning_tokens":377,"cache_read_input_tokens":256,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-05T23:11:15.163131+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Re-derive the occurrence rates from the same candidate list using an independent M dwarf temperature scale, such as bolometric fluxes or interferometric radii, and a separate completeness model, then check whether the turnover at 3750 K persists; if it shifts below roughly 3500 K or disappears, the claimed peak is not robust. The claim would also be weakened if a future uniformly selected transit survey of mid-to-late M dwarfs finds sub-Neptune occurrence staying flat or rising.","supporting_citations":[],"review_version":1}