{"id":"5e3da710-3d90-4690-8210-9dbf9665156f","arxiv_id":"2412.03416","paper_version":2,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":3,"one_line_summary":"After excluding super-Jupiters, transiting Jupiter-sized exoplanets have similar average masses around M-dwarf and FGK stars, with the difference driven by a scarcity of super-Jupiters around low-mass stars.","lead":"This paper compares the masses of transiting giant planets around M-dwarf and FGK stars. It finds that once super-Jupiters are removed, Jupiter-sized planets have similar average masses across stellar mass, suggesting a common formation threshold.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"Result 2 rests on an unquantified selection function and a data-dependent 2 MJ cut; with ~20 M-dwarf planets, failing to reject independence is not positive evidence for the title's claim.","rationale":"The reader's weakest assumption is exactly the load-bearing issue: Section 2.2 assumes the conditional mass distribution is unbiased despite heterogeneous selection and the requirement of published masses. I agree and sharpen the concern in three ways: the §2.2 defense evaluates measurement precision rather than the follow-up/publication trigger; the 2 MJ cutoff is chosen after inspecting the data and is not a pre-specified hypothesis; and with roughly 20 M-dwarf planets, a null EMD/t-test result is low-powered and cannot support the affirmative statement in the title. The paper honestly acknowledges the small sample and heterogeneous selection in Section 5.1, so the correct verdict remains conditional: the analysis is a useful and plausible first look, but the central claim needs a selection-function-controlled dataset or an explicit demonstration that follow-up incompleteness cannot mimic the result.","tokens_in":15093,"tokens_out":8796,"duration_ms":99002,"concrete_test":"Build a controlled subsample from a single TESS survey: all planets with Rp between 0.8 and 1.2 RJ and P<10 d around M and FGK stars, with RV follow-up to a fixed K threshold (e.g., K>20 m/s) and published non-detections included; fit f(Mp|Rp, M*) by survival analysis. If the M-dwarf and FGK medians below 2 MJ differ by more than the quoted 10%, or if the posterior on their difference excludes zero, the result is a selection artifact. If the medians agree within uncertainties, the selection concern is retired.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Result 2 in Section 4 asserts that f(Mp|Rp≈1 RJ, M*) is independent of stellar mass once planets above 2 MJ are excluded. The load-bearing condition is that the observed, mass-limited sample is an unbiased draw from this conditional distribution. That condition is not established. The sample is restricted to planets with published >3σ mass measurements. Follow-up and publication are not randomized: for FGK stars the archive contains many Jupiter-radius transiting candidates without RV masses, and follow-up is systematically allocated to high-K, hence on average more massive, planets; for M dwarfs the transiting GEMS census is small and more complete. Thus P(observed | Mp, Rp, M*) depends on Mp and M*, and the §2.2 argument (K≳50 m/s for a median FGK planet) addresses measurement precision, not the follow-up/publication trigger. The paper itself concedes in §5.1 that the FGK sample has a heterogeneous selection function. Additionally, the 2 MJ threshold is selected after seeing the data: 4 MJ leaves a residual bimodality, while 1.5–2 MJ removes it. Testing at a threshold chosen from the same data inflates the chance of a null finding, and with only ~20 M-dwarf planets, failing to reject is low-power evidence, not positive evidence of equality. A non-rejection cannot carry the title's positive claim unless the selection function is quantified.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper compares the bulk properties of transiting giant planets (Rp ≳ 8 R⊕) around FGKM host stars using archival data from the NASA Exoplanet Archive, supplemented by recent GEMS discoveries. It applies the MRExo nonparametric density estimator in two and three dimensions, conditions the 3D distribution at Rp = 1 RJ, and uses Earth-mover distance and Welch's t-test with bootstrap resampling to compare conditional planet-mass distributions across stellar mass. The two central results are: (1) including all planets, the average mass of Jupiter-sized planets around M dwarfs is lower than around FGK stars, driven by a scarcity of super-Jupiters (≳2 MJ) around M dwarfs; and (2) after excluding planets above 2 MJ, the average masses of Jupiter-sized planets appear independent of stellar mass from 0.4 to 1.6 M☉. The paper proposes a minimum disk dust mass threshold for Jovian formation via core accretion and tentatively discusses an abrupt change in the super-Jupiter-to-Jupiter ratio near the Kraft break, attributing it to a possible vsini-related detection bias.","tokens_in":15409,"tokens_out":4560,"duration_ms":45256,"significance":"If the second result is robust, it would provide an important empirical constraint on giant planet formation: the final masses of close-in Jupiters would be largely independent of stellar mass once the rare super-Jupiter population is removed, with the stellar-mass dependence appearing mainly in occurrence rates. The paper has genuine strengths: the use of MRExo, EMD, and Welch tests is appropriate for comparing normalized conditional distributions; the bootstrap resampling is a reasonable way to propagate finite-sample uncertainty; and the super-Jupiter scarcity around M dwarfs is an interesting empirical pattern visible already in Figure 1d. The discussion candidly recognizes many caveats, especially in Section 5.1. However, the central claim of mass independence is a positive statement built on a failure to reject the null in a small sample, under an unquantified selection function and with a mass cut chosen after inspecting the data. The evidence is therefore suggestive rather than conclusive, and the title/abstract overstate the current support.","major_comments":[{"comment":"The claim that f(Mp | Rp ≈ 1 RJ, M*) is unbiased with respect to stellar mass is not established. The sample requires published >3σ mass measurements, and the FGK and M-dwarf samples come from different surveys with different follow-up and publication histories. The argument in Section 2.2 that a median FGK planet would have K ≳ 50 m/s addresses measurement precision once RV data are obtained, not the probability that a target is selected for RV follow-up or that a mass measurement is published. The paper itself concedes in Section 5.1 that the FGK transiting giant planet sample has a heterogeneous selection function. A quantitative selection function, or at least a demonstration that the mass distributions of planets with and without published masses are consistent, is needed before Result 2 can be interpreted as a physical statement rather than a statement about the observed sample.","section":"Section 2.2 and Result 2 (Section 4)"},{"comment":"The 2 MJ threshold is introduced after inspecting the data: the text describes starting from the 4 MJ literature cut, finding a residual bimodality, then reducing the cutoff from 4 MJ to 2 MJ, and noting that 1.5 MJ gives a similar conclusion. Evaluating the null hypothesis at a threshold chosen from the same data inflates the chance of a non-rejection, and with roughly 20 M-dwarf planets a failure to reject is low-power evidence. The manuscript should either justify the threshold from an independent sample or present the test as exploratory; in either case, a power calculation is needed to state what difference would have been detectable.","section":"Section 3.1.2 and Result 2 (Section 4)"},{"comment":"The title's positive claim of similarity rests on a null result in a small sample. Section 5.1 notes that only about 20 GEMS are used, with about 5 below 0.5 M☉, and Figure 6 cautions against interpreting trends around these lowest-mass stars. The EMD and Welch tests reject the all-planet case at the 3σ level, but for the <2 MJ subset the tests are not shown to have power to detect a plausible stellar-mass dependence. Consequently, 'do not seem to show a dependence' is a fair summary, but 'are independent of stellar mass' and the abstract's 'striking similarity' overstate the evidence. Please add a quantitative statement of the smallest mass offset or trend that the current sample could detect at, say, 90% power.","section":"Section 4, Section 5.1, and Figure 6"}],"minor_comments":[{"comment":"There is a typo: 'betea polynomials' should be 'beta polynomials'.","section":"Section 3.1"},{"comment":"'bootstrap the sample and estimate the conditional distributions a 100 times' should read '100 times'.","section":"Section 3.1.2"},{"comment":"The sentence 'Gravitational instability has been as a potential alternative to core-accretion' is missing a verb and should be rephrased.","section":"Section 1"},{"comment":"The sentence 'In the disk instability massive disks that are large and cool enough to initiate instabilities are required (Boss 1997, 2006; Boss & Kanodia 2023) necessitates.' is grammatically incomplete and should be revised.","section":"Section 5.2"},{"comment":"The abstract says 'over two dozen' transiting GEMS while Section 5.1 says 'only ∼20 transiting GEMS'; please reconcile the number.","section":"Abstract and Section 5.1"},{"comment":"The blue numerator/denominator labels for the super-Jupiter-to-Jupiter ratios are small and difficult to read; a table or larger font would improve clarity.","section":"Figure 7"}],"recommendation":"major_revision","confidential_remarks":"This is a thought-provoking single-author paper with an honest discussion of its own limitations, and the raw empirical pattern — the scarcity of super-Jupiters around M dwarfs — is likely publishable. My reservations concern the strength of the headline claim relative to the evidence: the positive statement of mass independence rests on a null result under an unquantified selection function and a data-dependent mass cut. If the author reframes the title and abstract to match the exploratory nature of the <2 MJ comparison and adds the requested selection-function and power discussion, I would be supportive. The Kraft-break speculation is appropriately labeled as tentative."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Plain take: this is an honest, well-scoped observational comparison, but the title runs ahead of the evidence. The genuinely new piece is the conditional-mass analysis after dropping super-Jupiters: for transiting Jupiter-radius planets below 2 M_J, the data are consistent with planet mass independent of stellar mass over 0.4–1.6 M_sun. That specific comparison is not in the cited literature, and the paper does it transparently—MRExo, EMD, Welch tests, bootstraps, and the small-sample limits are flagged. I also give the author credit for separating the full-sample trend (stellar-mass dependence driven by super-Jupiter scarcity) from the sub-2 M_J comparison, and for labeling the Kraft-break idea as tentative rather than a result.\n\nThe soft spots are real but not fatal. The central claim is a non-rejection of the null after the mass cut is chosen from the same data: 4 M_J leaves a residual bimodality, so the cut is lowered to 2 M_J or 1.5 M_J. With roughly 20 transiting GEMS, and about 5 below 0.5 M_sun, failing to reject is low-power evidence, not positive evidence of equality. The more serious concern is selection. The sample requires published >3-sigma masses, and follow-up/publication is not a random draw from f(M_p | R_p, M*). The Section 2.2 argument (a median FGK planet would have K ~ 50 m/s) addresses measurement detectability, not the trigger that got masses published; the author himself concedes the FGK sample has a heterogeneous selection function in Section 5.1. That does not kill the empirical comparison—the sub-2 M_J medians really do look close—but it means the title's positive claim is not yet established. The minimum-disk-mass explanation is plausible and connects nicely to occurrence-rate trends, but it is a hypothesis rather than a tested model.\n\nWho is this for? Planet-formation theorists and observers designing M-dwarf RV follow-up. It deserves a serious referee rather than a desk reject. The analysis is careful, the empirical contrast is worth publishing, and the limitations are mostly on the table. I would ask for a revised title and abstract that mention the mass cut, a sensitivity statement showing how the conclusion changes across thresholds, and either a selection-function analysis or a stronger, front-loaded caveat. I would cite it only as a tentative small-sample comparison, not as a measured fact.","headline":"A legitimate, clearly-scoped empirical comparison whose headline overstates the evidence; the sub-2 M_J mass independence is a useful tentative result, not an established fact.","tokens_in":15897,"tokens_out":2108,"would_cite":true,"duration_ms":22257,"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 that the lower average mass of M-dwarf Jupiters comes from a scarcity of super-Jupiters; below 2 Jupiter masses, Jupiter-sized planets have the same mass whether they orbit a 0.4 or a 1.6 solar-mass star.","keywords":["giant planets","M-dwarf planets","super-Jupiters","exoplanet masses","transiting exoplanets","core accretion","protoplanetary disk mass","planet occurrence"],"falsifier":"Conduct a homogeneous radial-velocity confirmation campaign for transiting Jupiter-radius candidates around stars spanning 0.4 to 1.6 solar masses, with the same follow-up threshold and published non-detections; if after excluding planets above 2 Jupiter masses the median masses of the M-dwarf and FGK subsamples differ by more than the roughly 10 percent seen in the current comparison, or the Earth-mover distance again rejects stellar-mass independence at the 3-sigma level, the central claim is falsified.","tokens_in":14913,"feed_emoji":"🪐","tokens_out":8428,"duration_ms":73895,"temperature":0.7,"pith_summary":"This paper asks whether giant planets around low-mass stars are fundamentally different from those around Sun-like stars, and answers that for Jupiter-sized transiting planets the answer is no. Using a sample of roughly 550 well-characterized transiting giant planets, it reconstructs the conditional distribution of planet mass given planet radius and stellar mass. The analysis finds that the lower average mass of M-dwarf Jupiters is driven almost entirely by a scarcity of super-Jupiters above about two Jupiter masses. Once planets above 2 Jupiter masses are removed, the mass distributions of Jupiter-radius planets around host stars from 0.4 to 1.6 solar masses are statistically indistinguishable. The paper proposes a minimum disk dust mass threshold for Jovian core accretion as the explanation, which also accounts for the lower occurrence of giant planets around M-dwarfs.","feed_headline":"M-dwarf Jupiters match FGK warm-Jupiters below 2 Jupiter masses","feed_subtitle":"A 548-planet sample shows the average mass gap vanishes once super-Jupiters are excluded.","key_machinery":"The carrying object is the paper's n-dimensional nonparametric density model, which approximates the joint distribution of planet mass, planet radius, and stellar mass as a sum of beta-density polynomial basis functions convolved with normal kernels to carry measurement uncertainties, with the polynomial complexity selected by 10-fold cross-validation. Conditioning this joint density at one Jupiter radius yields the normalized conditional distribution of planet mass as a function of stellar mass, allowing the paper to compare planet masses across host stars without depending on absolute occurrence rates. The comparison tools are the Earth-mover (Wasserstein) distance and Welch's t-test applied to bootstrapped conditional distributions, supplemented by a Gaussian kernel-density histogram comparison of M-dwarf and FGK subsamples. The interpretive mechanism proposed is a minimum disk dust mass threshold for Jovian formation through core accretion, illustrated with measured disk dust-mass distributions.","core_discovery":"The paper's central result is that after accounting for the stellar-mass-dependent prevalence of super-Jupiters by excluding planets above 2 Jupiter masses, the average mass of Jupiter-sized transiting planets is independent of stellar mass between 0.4 and 1.6 solar masses. This is established by fitting a three-dimensional nonparametric density to planet mass, planet radius, and stellar mass, conditioning the density at one Jupiter radius, and comparing the resulting conditional mass distributions with the Earth-mover distance and Welch's t-test. Before the cut, the conditional distributions differ at the 3-sigma level between the lowest-mass and solar-type hosts; after the cut, the null hypothesis of independence cannot be rejected, and a direct M-dwarf versus FGK histogram comparison gives median masses within about 10 percent. The paper interprets this as evidence that stellar mass sets the probability of forming a giant planet but not the typical mass of the Jupiters that do form, and it ties that interpretation to a minimum disk dust mass required for core accretion.","pith_inferences":["If the minimum-disk-mass explanation is correct, the disks that do form Jupiters around M-dwarfs should have dust masses comparable to the disks around FGK hosts of Jupiters, not scaled down with stellar mass; a disk survey of stars hosting these planets could test this directly.","Re-running the same conditional-density comparison with per-planet selection weights accounting for each survey's radial-velocity follow-up threshold would show whether the below-2-Jupiter-mass convergence survives a formal completeness correction, a test the current heterogeneous sample cannot perform.","Because the paper treats bulk density as a proxy for bulk metallicity, the flat mass trend hints that atmospheric metallicity measurements of M-dwarf giants and FGK warm Jupiters may also look similar; this is a natural follow-up that the paper does not itself claim.","A homogeneous radial-velocity survey of transiting warm Jupiters around F stars on both sides of the Kraft break would settle whether the super-Jupiter ratio jump is astrophysical or a rotational-broadening artifact."],"forward_implications":["Below about 2 Jupiter masses, a Jupiter-radius transiting planet has the same average mass and bulk density around host stars from 0.4 to 1.6 solar masses.","The lower average mass of M-dwarf Jupiters in the full sample is a population effect: super-Jupiters are rarer around lower-mass stars, not that the Jupiters that do form are lighter.","A minimum disk dust mass threshold for core accretion would simultaneously explain the declining occurrence of giant planets with stellar mass and the flat mass of the Jupiters that do form.","The apparent jump in the super-Jupiter-to-Jupiter ratio near 1.3 solar masses, close to the Kraft break, is currently tentative and could be a rotation-related detection bias; a controlled sample with published non-detections is needed to confirm it.","The sample of planets around stars below about 0.5 solar masses is only about five objects, so the paper's conclusions should not yet be extended to the lowest-mass M-dwarfs."],"supporting_citations":[{"why":"Supplies the Planetary Systems Table queried for the 548-planet sample and the stellar and planetary mass and radius measurements.","marker":"NASA Exoplanet Archive 2024"},{"why":"Defines the survey design, the giant-planet radius cut, and the methodology for comparing conditional distributions of planet properties.","marker":"Kanodia et al. 2024a"},{"why":"Provides the multi-dimensional joint-distribution inference framework used to estimate the mass-radius-stellar-mass density.","marker":"Kanodia et al. 2023a"},{"why":"Provides the nonparametric beta-density basis functions and cross-validation approach that the inference framework builds on.","marker":"Ning et al. 2018"},{"why":"Supplies one empirical basis for separating super-Jupiters from Jupiters by mass in the sample filtering.","marker":"Santos et al. 2017"},{"why":"Provides the second empirical distinction between Jupiters and super-Jupiters used to justify the mass cut.","marker":"Schlaufman 2018"},{"why":"Provides the Lupus disk dust-mass distributions that ground the proposed minimum-disk-mass threshold for Jovian formation.","marker":"Ansdell et al. 2016"},{"why":"Represents the core-accretion population synthesis prediction that lower-mass stars should host lower-mass giants, which the paper's flat mass trend contrasts with.","marker":"Ida & Lin 2005"},{"why":"Defines the Kraft break in stellar rotation that frames the tentative transition in the super-Jupiter-to-Jupiter ratio.","marker":"Kraft 1967"},{"why":"Defines the Earth-mover distance used to compare the conditional planet-mass distributions across stellar mass.","marker":"Rubner et al. 1998"}],"fun_headline_variants":["Without super-Jupiters, M-dwarf and FGK Jupiters share similar masses","Excluding super-Jupiters, M-dwarf Jupiters match FGK warm-Jupiters","Super-Jupiters drive mass gap; typical Jupiters are same across stars","Cut super-Jupiters, M-dwarf Jupiters match FGK warm-Jupiters","M-dwarf Jupiters weigh like FGK warm-Jupiters once super-Jupiters are excluded"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The central assumption is that the published sample is an unbiased draw of planet masses at fixed radius and stellar mass, so a planet of a given mass around an M-dwarf is just as likely to receive a published mass measurement as one around an FGK star, and the paper does not provide a quantitative selection function to back this.","fun_headline_variants_meta":{"raw":{"variants":["Without super-Jupiters, M-dwarf and FGK Jupiters share similar masses","Excluding super-Jupiters, M-dwarf Jupiters match FGK warm-Jupiters","Super-Jupiters drive mass gap; typical Jupiters are same across stars","Cut super-Jupiters, M-dwarf Jupiters match FGK warm-Jupiters","M-dwarf Jupiters weigh like FGK warm-Jupiters once super-Jupiters are excluded"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000711,"raw_usage":{"total_tokens":3246,"prompt_tokens":1037,"completion_tokens":2209,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":653,"completion_tokens_details":{"reasoning_tokens":2089}},"tokens_in":653,"tokens_out":2209,"duration_ms":14216,"temperature":1.0,"reasoning_tokens":2089,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-11T22:24:31.931445+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Conduct a homogeneous radial-velocity confirmation campaign for transiting Jupiter-radius candidates around stars spanning 0.4 to 1.6 solar masses, with the same follow-up threshold and published non-detections; if after excluding planets above 2 Jupiter masses the median masses of the M-dwarf and FGK subsamples differ by more than the roughly 10 percent seen in the current comparison, or the Earth-mover distance again rejects stellar-mass independence at the 3-sigma level, the central claim is falsified.","supporting_citations":[{"cited_title":"2018, ApJ, 869, 5","cited_arxiv_id":null,"evidence_quote":"Provides the nonparametric beta-density basis functions and cross-validation approach that the inference framework builds on."},{"cited_title":"C., Adibekyan, V., Figueira, P., et al","cited_arxiv_id":null,"evidence_quote":"Supplies one empirical basis for separating super-Jupiters from Jupiters by mass in the sample filtering."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Provides the second empirical distinction between Jupiters and super-Jupiters used to justify the mass cut."},{"cited_title":"P., van der Marel, N., et al","cited_arxiv_id":null,"evidence_quote":"Provides the Lupus disk dust-mass distributions that ground the proposed minimum-disk-mass threshold for Jovian formation."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Represents the core-accretion population synthesis prediction that lower-mass stars should host lower-mass giants, which the paper's flat mass trend contrasts with."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Defines the Kraft break in stellar rotation that frames the tentative transition in the super-Jupiter-to-Jupiter ratio."},{"cited_title":"1998, in Sixth International Conference on Computer Vision (IEEE Cat","cited_arxiv_id":null,"evidence_quote":"Defines the Earth-mover distance used to compare the conditional planet-mass distributions across stellar mass."}],"review_version":1}