{"id":"d6992c7c-4014-4cf2-9dfe-45032108de98","arxiv_id":"2602.11017","paper_version":2,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":3,"one_line_summary":"Hot super-Earths are about eight times more common around stars with a cold Jupiter than around typical field stars.","lead":"This paper searched TESS transit data for 132 stars already known to host a cold Jupiter and found five hot super-Earths where only about 0.6 were expected, implying cold Jupiters boost hot super-Earth occurrence by roughly a factor of eight. It is one of the first direct, completeness-corrected measurements of the super-Earth–cold Jupiter correlation and informs how planetary systems assemble.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The 87% system fraction rests on an admitted unknown: the raw in-sample multiplicity 5/4 is used without completeness correction, and P(HSE|CJ)=η/m is highly sensitive to m.","rationale":"The reader's inclination concern is legitimate but bounded: a plausible RV-selection alignment bias could raise Nbar from 0.58 to perhaps 1.0-1.2, which would reduce f from 8.1 to roughly 5-7 and weaken the 99.9% statement to about 99%, but not overturn the core 'enhancement' conclusion. The more load-bearing issue for the headline 'nearly all CJ hosts have HSEs' claim is the multiplicity correction. The paper itself admits the average hot-super-Earth multiplicity is unknown, and using the raw 5/4 from the detected sample is not a completeness-corrected estimate. Since the system fraction is directly proportional to 1/m, small changes in m change the 87% number dramatically. This does not invalidate the occurrence-enhancement result, so the appropriate verdict remains CONDITIONAL, unchanged from the reader's assessment. The proposed test would settle whether the 87% system fraction is supported or should be replaced by a substantially lower, more conservative estimate.","tokens_in":19471,"tokens_out":18592,"duration_ms":190492,"concrete_test":"Obtain an independent, completeness-corrected multiplicity distribution for hot super-Earths (P<10 d, 1-4 R⊕) from Kepler multi-transiting systems, or run a dedicated TESS injection-recovery search for additional transits in the four HSE-hosting systems to estimate the true conditional multiplicity m. Then recompute P(HSE|CJ)=η(HSE|CJ)/m with η fixed at the paper's 1.09. If m is consistent with 1.25, the 87% claim survives; if m>1.5, the headline system fraction should be revised substantially downward.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central enhancement factor f=8.1 is reasonably robust: even a factor-of-two upward revision of Nbar from alignment/inclination effects would leave f>4 and still statistically significant. The more fragile load-bearing step is the multiplicity correction in §5, Eq. (8). The paper explicitly states that the average multiplicity of hot super-Earths is unknown, then adopts the raw observed value 5/4=1.25 from the four HSE-hosting systems. This is not a completeness-corrected multiplicity: it counts only the transiting HSEs actually detected and ignores non-transiting companions in those systems, so it is a lower bound on the true conditional multiplicity. Because P(HSE|CJ)=η(HSE|CJ)/m with η≈1.09, the 87% result is extremely sensitive: m=1.4 gives 78%, m=2 gives 55%, m=3 gives 36%. The abstract's 91% vs the full-text 87% further highlights the fragility. The f result does not depend on this step, but the 'nearly all CJ hosts have HSEs' conclusion—highlighted in §6.1—is directly built on this unvalidated estimate. The paper's system-fraction claim therefore rests on an admitted unknown, not on a measured quantity.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek-v4-flash","summary":"This paper constructs a sample of 132 Sun-like stars with RV-detected cold Jupiters, performs a uniform TESS transit search for inner hot super-Earths (1–4 R⊕, P<10 d), and validates two candidates around HD 50554. After injection-recovery completeness and geometric transit probabilities, 5 detected HSEs are compared with an expected field background of Nbar=0.58 from Kepler occurrence rates. A Poisson/Gamma model gives an enhancement factor f=8.1^{+4.3}_{-3.2} with P(f≤1)=0.1%. Dividing the conditional occurrence rate η=1.09 by an assumed multiplicity 5/4 yields a system fraction P(HSE|CJ)≈87%. The paper also explores metallicity and mass sub-samples.","tokens_in":19797,"tokens_out":15886,"duration_ms":147175,"significance":"If correct, this is a direct, well-defined measurement of the inverted conditional probability P(SE|CJ), strongly supporting a positive SE–CJ correlation and providing a useful constraint on formation and dynamical-evolution models. Strengths include the clean RV-selected CJ sample with explicit exclusion criteria, a uniform TESS BLS search with injection-recovery completeness, careful validation of the HD 50554 candidates using photometry, RV, and Gaia astrometry, and transparent Poisson statistics with robustness checks against two independent field occurrence maps and alternative CJ definitions. The core enhancement-factor result is largely independent of the multiplicity step; the system-fraction claim is not.","major_comments":[{"comment":"The system fraction P(HSE|CJ)≈87% is obtained by dividing η(HSE|CJ)=1.09 by the raw observed multiplicity 5/4=1.25. The text admits the average multiplicity of hot super-Earths is not known. Because 5/4 counts only transiting HSEs actually detected and ignores non-transiting companions and detection incompleteness, it is a lower bound on the true mean multiplicity among HSE hosts. Since P(HSE|CJ)=η/m, using a lower bound for m yields an upper bound on the system fraction: m=2 gives about 55%, and the value ~3 cited in the text gives about 36%. The 87% claim, highlighted in the abstract and §6.1, is therefore not supported as an estimate. Please provide a completeness-corrected multiplicity estimate or explicitly present the result as a sensitivity/upper bound. The supplied abstract's 91% versus §5's 87% must also be reconciled.","section":"§5, Eq. (8) and §6.1"},{"comment":"The geometric transit probability assumes isotropic inner HSE inclinations. If inner orbits are preferentially aligned with the RV-detected CJ, and if RV detection favors sin i≈1, the effective p_tr is larger than 0.9 R*/a, raising Nbar in Eq. (4) and lowering f. The text acknowledges this possibility and cites large mutual inclinations in π Men and HD 50554, but it does not quantify the effect. Please add a numerical sensitivity test (e.g., a mutual-inclination distribution or a uniform upward factor on p_tr) and propagate the resulting change into f and the formal significance.","section":"§3.2, Eq. (2)"},{"comment":"The posterior for f treats Nbar=0.58 as fixed. Nbar inherits uncertainty from the external Kepler occurrence map and from the injection-recovery efficiency map, yet the quoted 68% interval and the p<0.001 statement reflect only Poisson counting noise in N=5. Please marginalize over the uncertainty in Nbar, or at least show how P(f≤1) changes under conservative upward revisions of Nbar (e.g., the 1.3× metallicity correction and a factor-of-two alignment correction). This is needed to support the formal 99.9% claim.","section":"§5, Eq. (6)"}],"minor_comments":[{"comment":"The opening abstract block reports f=6.5^{+3.1}_{-2.3} and a 91% system fraction, while the full-text abstract, §5, and §6.1 report f=8.1^{+4.3}_{-3.2} and 87%. These headline numbers must be aligned before publication.","section":"Abstract/full text"},{"comment":"The Gamma posterior shape parameter is written as N_NSE+1; this should be N_HSE+1.","section":"Eq. (6)"},{"comment":"The summary states 'radii of 1.3M⊕ and 1.4M⊕'; the units should be R⊕.","section":"§6.1"},{"comment":"The mass quoted for π Men b, ≈14 M_J, appears inconsistent with the inclination of ≈54° cited in the same paragraph and with published RV minimum masses. Please verify the value and source.","section":"§6.2.3"},{"comment":"The right-panel colorbar label 'Pdet Ptr' should read 'Pdet × Ptr'. In Table 3, the format of the mass upper limits (Mp <5.3 and <10.4 M⊕) is unclear and should be clarified.","section":"Figure 3 / Table 3"}],"recommendation":"major_revision","confidential_remarks":"The core enhancement-factor result, f≈8 with strong rejection of f≤1, is credible and likely publishable after revision. The most important fix is the multiplicity step behind the 87% system-fraction claim, which currently rests on an admitted unknown and is an upper bound rather than an estimate. The abstract inconsistency and the unquantified geometric/inclination assumption also need attention. I do not recommend rejection: the main claim is robust to the identified issues and the multiplicity problem can be addressed with a sensitivity analysis or a reframed conclusion."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Colleague,\n\nThis paper is worth your time. It gives the first TESS-based, completeness-corrected direct measurement of hot super-Earth occurrence in RV-selected cold-Jupiter systems. The headline result—about an 8x enhancement over the field—holds up under both external occurrence maps (8.1 and 10.7), and the null is rejected at 99.9%. The Poisson derivation is clean, the pipeline work is careful, and the HD 50554 validation is solid. I disagree with the reader's emphasis: the inclination assumption is a minor concern, not the load-bearing one. Even a factor-of-two change in N_bar leaves f>4 and still significant. The qualitative correlation is not in doubt.\n\nThe genuine soft spot is the system fraction. The 87% P(HSE|CJ) comes from dividing eta=1.09 by an adopted multiplicity m=1.25, which is just the raw 5/4 detections from four systems. That is a lower bound on the true multiplicity, not a completeness-corrected value. The paper itself states the average HSE multiplicity is unknown, then treats 5/4 as appropriate. With m=2, the fraction drops to 55%; m=3 gives 36%. So the 'nearly all CJ hosts have HSEs' conclusion—the most memorable line in the paper—is an upper limit built on an admitted unknown. The abstract's 91% versus the full text's 87% underscores the fragility. That needs to be reconciled and the multiplicity step replaced with a proper completeness correction or a sensitivity analysis.\n\nThe isotropic-inclination assumption for p_tr is a legitimate uncertainty, but the paper handles it honestly and the two dynamically hot systems it highlights (pi Men, HD 50554) suggest the assumption is conservative, not aggressive. I would not block on it.\n\nThe citation pattern looks normal—they compare directly with Herman et al. and Rosenthal et al., explain the differences in sample definitions, and do not overstate what those papers did. The work is transparent and the central claim is convincing given N=5 and N_bar=0.58. It deserves a serious referee, but a referee should push hard on the multiplicity correction and the abstract/full-text mismatch.\n\nSend it to review.","headline":"The core enhancement factor (~8x) is credible and novel, but the 87% system fraction is an upper limit built on an admitted unknown multiplicity, and the abstract/full-text numbers disagree.","tokens_in":20301,"tokens_out":3407,"would_cite":true,"duration_ms":29609,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"Stars that host a distant Jupiter-mass planet are about eight times more likely to also host a close-in super-Earth, according to a transit survey of 132 known cold-Jupiter systems.","keywords":["cold Jupiters","hot super-Earths","occurrence rates","TESS","radial velocity planets","transit search","mutual inclinations","planet formation"],"falsifier":"Measure the mutual inclinations between hot super-Earths and their outer cold Jupiters in a statistically meaningful sample—using transit-duration ratios, Rossiter–McLaughlin observations, or astrometry. If typical mutual inclinations are small (≲5°) and RV-selected cold Jupiters are preferentially edge-on, the isotropic-transit assumption fails and the enhancement factor is overestimated; if mutual inclinations are large, the enhancement would be even larger. A pipeline-independent check is to run the same TESS search on a metallicity- and brightness-matched sample of field stars without cold","tokens_in":19326,"feed_emoji":"🪐","tokens_out":9393,"duration_ms":85837,"temperature":0.7,"pith_summary":"This paper attempts to measure, directly, how often a star that hosts a distant Jupiter-mass planet (a cold Jupiter) also hosts a close-in super-Earth. Using TESS transit data for 132 Sun-like stars with known radial-velocity cold Jupiters, the authors find five transiting hot super-Earths (planets of 1–4 Earth radii with periods under 10 days) around four stars. After correcting for geometric transit probability and detection sensitivity, they report that cold Jupiters enhance the occurrence rate of hot super-Earths by a factor of 8.1 (68% interval +4.3/−3.2), excluding 'no enhancement' at 99.9% confidence, and that about 87–91% of cold-Jupiter systems host at least one hot super-Earth. If correct, this converts a previously Bayesian conjecture—that nearly all cold-Jupiter hosts also harbor inner super-Earths—into a direct observational measurement, sharpening constraints on planet-formation and system-architecture models.","feed_headline":"Cold Jupiters make hot super-Earths 8x likelier","feed_subtitle":"Five close-in super-Earths found among 132 distant-giant systems where only one was expected.","key_machinery":"The load-bearing quantity is the enhancement factor f = η(HSE|CJ)/η(HSE), estimated from the ratio of the five observed transiting hot super-Earths to N̄ = 0.58, the expected number under the null hypothesis. Equation (4) builds N̄ by summing over orbital-period and radius bins the field occurrence rate times the geometric transit probability p_tr = 0.9 R*/a and the pipeline detection efficiency, the latter measured by injecting 200 synthetic transits around each star and recovering them with a BLS search. The posterior on f is a Gamma distribution arising from a Poisson likelihood for the detection count. The geometric transit probability, which assumes isotropic inner-planet inclinations,","core_discovery":"On the paper's own terms, the central discovery is that the conditional occurrence of hot super-Earths in cold-Jupiter systems, η(HSE|CJ), exceeds the field rate η(HSE) by an order of magnitude. The authors compute the expected number of transiting hot super-Earths in their 132-star sample under the null hypothesis of no correlation, N̄ = 0.58, using Kepler-based field occurrence rates and per-star transit and detection efficiencies determined from injection-recovery simulations. With five planets observed, the Poisson-based posterior gives the enhancement factor f = 8.1^{+4.3}_{-3.2}, and P(f ≤ 1) = 0.1%. Dividing the implied conditional occurrence rate by the sample's average multiplicity","pith_inferences":["If the isotropic-inclination assumption is wrong and inner super-Earths preferentially align with the cold Jupiter's orbital plane (while RV detection favors edge-on giants), the true transit probability is higher than assumed; N̄ would rise and the 8.1× enhancement would shrink. Mutual-inclination measurements could separate a genuine occurrence boost from an architecture-alignment effect.","The abstract reports 91% for P(HSE|CJ) while Section 5 and the summary give 87%; the derivation in Eq. (8) uses the sample's average multiplicity, making 87% the better documented figure. The mismatch is not reconciled in the text.","The detection-efficiency map rests on injection-recovery without visual validation of recovered signals; the authors argue the sample is clean, but any residual false-positive rate would bias N̄ and hence f. An independent re-analysis of the same 132 light curves with a different pipeline would test the robustness.","The apparent enhancement in the metal-poor subsample (1 of 43 systems) suggests the correlation may not be purely metallicity-driven; extending this TESS-based approach to a larger sample of giants found astrometrically at low metallicity would test whether the boost persists."],"forward_implications":["Occurrence-rate models and planet-formation simulations must reproduce an order-of-magnitude enhancement of close-in super-Earths when an outer giant is present, rather than treating the two populations as independent.","RV-only surveys systematically miss most inner super-Earths in cold-Jupiter systems; combined transit+RV samples are necessary to measure P(SE|CJ), which explains part of the scatter among earlier correlation studies.","The large mutual inclinations seen in the two super-Jupiter systems in this sample show that the inner and outer planets need not be coplanar, so the enhancement is a genuine occurrence effect rather than purely a geometric alignment artifact—though the size of the effect still depends on the inclination distribution.","Targeted searches for transits around known RV giant hosts can be an efficient way to build a statistical sample of multi-planet architectures, since each detected inner planet is a nearly guaranteed co-existing system."],"fun_headline_variants":["Cold Jupiters boost hot super-Earths 8-fold","Hot super-Earths 8x likelier with cold Jupiters","Cold Jupiters yield 8x more hot super-Earths","8x more hot super-Earths around cold Jupiters"],"cache_read_input_tokens":2304,"weakest_assumption_plain":"The assumption that the inner super-Earths' orbital inclinations are distributed isotropically, so that p_tr = 0.9 R*/a applies unconditionally, is the load-bearing premise: if inner planets preferentially share the cold Jupiter's orbital plane, the assumed transit probability is too low, N̄ is underestimated, and the measured 8.1× enhancement would shrink.","fun_headline_variants_meta":{"raw":{"variants":["Cold Jupiters boost hot super-Earths 8-fold","Hot super-Earths 8x likelier with cold Jupiters","Cold Jupiters yield 8x more hot super-Earths","8x more hot super-Earths around cold Jupiters"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000656,"raw_usage":{"total_tokens":2900,"prompt_tokens":864,"completion_tokens":2036,"prompt_tokens_details":{"cached_tokens":256},"prompt_cache_hit_tokens":256,"prompt_cache_miss_tokens":608,"completion_tokens_details":{"reasoning_tokens":1958}},"tokens_in":608,"tokens_out":2036,"duration_ms":15231,"temperature":1.0,"reasoning_tokens":1958,"cache_read_input_tokens":256,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-03T00:53:48.816656+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Measure the mutual inclinations between hot super-Earths and their outer cold Jupiters in a statistically meaningful sample—using transit-duration ratios, Rossiter–McLaughlin observations, or astrometry. If typical mutual inclinations are small (≲5°) and RV-selected cold Jupiters are preferentially edge-on, the isotropic-transit assumption fails and the enhancement factor is overestimated; if mutual inclinations are large, the enhancement would be even larger. A pipeline-independent check is to run the same TESS search on a metallicity- and brightness-matched sample of field stars without cold","supporting_citations":[],"review_version":1}