REVIEW 2 major objections 6 minor 299 references
The GAPS Programme with HARPS-N at TNG LXXVII. Occurrence rates of small close-in planets in the presence of cold Jupiters
T0 review · 2 major / 6 minor · reviewed 2026-07-14 · grok-4.5
Pith's one-line read Outer cold Jupiters do not strongly promote or suppress inner small planets at average stellar mass and metallicity, but dynamically quiet giants leave room for more warm companions.
desk verdict Solid, homogeneous RV demographics paper that cleanly measures ISP rates around CJ hosts and finds no strong overall correlation at average metallicity/mass; the alim split is secondary and not load-bearing. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The dynamical-stability boundary alim = a1(1−e1)−2√3 RH, which folds the outer giant’s mass, semi-major axis and eccentricity into a single length that separates systems whose inner zones remain unperturbed from those that do not.
What would settle it
A larger, uniformly sampled set of cold-Jupiter hosts in which warm Neptunes appear at comparable rates on both sides of the alim = 1.5 au divide, or in which the conditional probability of an inner small planet given an outer giant rises well above the unconditional rate once completeness is properly accounted for.
Extended reading notes
Core claim
Around stars that already host cold Jupiters, the occurrence of small close-in planets is moderate (a few to roughly 15 percent depending on mass and period) and shows no strong overall correlation with the presence of the outer giant at average stellar metallicity and mass; the rates become significantly higher only when the outer giant leaves the inner region dynamically stable.
Load-bearing premise
The claim that a single cut at alim of 1.5 au cleanly divides systems into those whose outer giants leave the inner regions free of dynamical interference and those that do not.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper constructs a homogeneous sample of 137 FGK stars hosting cold Jupiters (CJs; a_peri > 1 au, m sin i > 0.1 M_J), of which 114 form a regular sample without inner giants and 23 host additional inner gas giants treated separately. Archival RVs from many instruments plus unpublished HARPS-N GAPS data are fitted uniformly with PyORBIT; six new candidates are reported (two flagged non-robust and excluded from statistics). Detection completeness is mapped with two independent injection-recovery codes that agree within 1–2σ, and occurrence rates of inner small planets (ISPs; 3 ≤ m sin i ≤ 31.7 M_⊕, P ≤ 400 d) are inverted as planets per star. Headline rates are ~5/13/12% for hot/warm/cool Neptunes and ~11/16% for hot/warm super-Earths; systems with a_lim ≥ 1.5 au show a significant excess of warm planets. Comparisons with Rosenthal et al. (2022) and Bonomo et al. (2023, 2025) via Bayes’ theorem indicate no strong ISP–CJ correlation at average stellar mass and metallicity, while hot-Jupiter rates in the full sample are formally ~2σ higher than literature field values.
Significance. If the rates and the lack of a strong ISP–CJ correlation hold, the work supplies one of the largest, most homogeneous RV-based conditional occurrence measurements for Solar-System-like architectures and helps resolve the tension between earlier claims of near-100% correlation and more recent null results. Strengths include dual-code cross-validation of completeness, explicit flagging of low super-Earth completeness and non-robust candidates, uniform re-analysis of multi-instrument data, and transparent literature comparisons that reuse external F_ISP and F_CJ. The a_lim dynamical-stability test quantifies an expected architectural dependence without being required for the headline rates. The result is of clear interest to formation and migration theory and to the design of future RV and transit surveys.
major comments (2)
- §7.2 and Eqs. (4)–(5): the warm-planet excess is reported only for the binary split a_lim ≥ 1.5 au (3.8σ for warm Neptunes). Because a_lim folds mass, eccentricity and semi-major axis into a single threshold, and multi-giant interactions are neglected by construction, a continuous or multi-threshold test (or a leave-one-out check on the 13 warm detections) would strengthen the claim that dynamical stability, rather than a correlated stellar property, drives the excess. The paper already notes that hot-planet rates are insensitive to the cut; extending that robustness statement to the warm bin would make the secondary result more secure.
- Table 1 and §7.1: cool super-Earth completeness is only 4.8% and warm-SE completeness 15.9%, with all three warm SEs coming from a handful of intensively monitored systems. The text correctly cautions that the SE rates should be taken carefully, yet they still appear in the abstract and conclusions at the same footing as the better-constrained Neptune rates. Either demote the SE numbers to upper limits / exploratory values or quantify the bias introduced by the best-sampled systems more explicitly (e.g., by a jackknife that removes HD 219134, HD 164922, etc.).
minor comments (6)
- Abstract vs. Table 1: abstract quotes ~5%, ~13%, ~12% (Neptunes) and ~11%, ~16% (SEs); Table 1 gives 4.9, 13.7, 10.1 and 11.5, 16.5. Align the rounded values or state that they are approximate.
- §2 criterion 1 and §7.3.1: CJ definition uses a_peri > 1 au here but a > 1 au (or 0.23–10 au) in some comparison works. A short explicit statement that the period-valley gap makes the difference negligible would help readers.
- Figure 5 caption and §4: state clearly which of the two codes produced the displayed map and note that the second code yields systematically lower low-mass completeness (already mentioned in text).
- Appendix A: for HD 204941 and HD 170469 the candidates are correctly excluded from statistics, but a one-sentence summary table of which new candidates enter the occurrence calculation would improve clarity.
- §7.4.1: the ~2σ excess of HJs relative to Howard et al. (2010) and Wittenmyer et al. (2020) is interesting; a brief note on whether the excess survives after removing the 23 systems that were selected precisely because they host inner giants would avoid any selection-loop concern.
- Typographical: “lanetary” → “planetary” (App. A, HD 204941); occasional “msini” vs “m sin i” inconsistency; “alim” sometimes written without subscript.
Circularity Check
No significant circularity: occurrence rates are inverted from observed counts plus independently computed completeness maps; literature comparisons use external benchmarks.
full rationale
The central derivation (Sect. 4 and 7) injects synthetic Keplerians into post-fit residuals on a period-mass grid, measures recovery fractions with two independent codes (BIC and FAP criteria), averages to a sample completeness map C, then inverts the Poisson (or binomial) distribution for η (or F) given the number of detections n. No free parameter is fitted to the target occurrence rates themselves, and the dual-code cross-check plus explicit low-completeness caveats for cool super-Earths keep the numbers self-contained. The alim dynamical cut (Eqs. 4–5) is a secondary post-hoc split that quantifies an expected warm-planet excess; it is not used to force the headline ISP–CJ rates or the Bayes conversion that recovers F_CJ|ISP. Self-citations (GAPS papers, Barbato et al. 2018, Bonomo et al. 2025) supply sample context or external F_CJ values but do not close a definitional loop on the new 114-star rates. The paper is therefore essentially non-circular.
Assumptions & free parameters
free parameters (4)
- alim threshold =
1.5 au
- eccentricity cut for subgroups =
0.3
- super-Jupiter mass cut =
4 MJ
- ISP mass/period bin edges =
as stated in §7.1
assumptions (4)
- domain assumption RV injection-recovery with fixed e = 0 and random epoch adequately measures completeness for low-mass short-period planets.
- domain assumption The Hill-radius stability limit alim = a(1−e)−2√3 RH correctly ranks dynamical influence of the outer giant on the inner system.
- domain assumption Stars with log R'HK < −4.8 and V < 10 are sufficiently inactive and bright for reliable low-mass planet searches.
- standard math Poisson/binomial inversion of counts and average completeness yields unbiased occurrence rates.
Cite this review
Pith. "Pith review of The GAPS Programme with HARPS-N at TNG LXXVII. Occurrence rates of small close-in planets in the presence of cold Jupiters." pith.science (2026). https://pith.science/paper/3MD5FAOE
@misc{pith2026260709320,
author = {Pith},
title = {Pith review of: The GAPS Programme with HARPS-N at TNG LXXVII. Occurrence rates of small close-in planets in the presence of cold Jupiters},
year = {2026},
howpublished = {\url{https://pith.science/paper/3MD5FAOE}},
note = {Machine review of arXiv:2607.09320}
}
abstract
Context. The architecture of our Solar System, with inner small planets (ISPs) and outer giants, may or may not be common. Understanding whether a correlation exists between ISPs and outer cold giants is key to evaluating how common systems with a similar architecture to our own are. Aims. This study aims to build a large, homogeneous sample of systems hosting cold Jupiters (CJs, a > 1 au, msini > 0.1 M$_J$) detected via radial velocities (RVs), and to assess the presence of additional ISPs (P < 400 d, 3 < msini < 31.7 M$_{\oplus}$), studying the correlation between these two types of objects. Methods. We selected 137 stars known to host a CJ, including 23 which also harbor a hot Jupiter and were treated separately. Data from various instruments were compiled, including unpublished data gathered with HARPS-N within the GAPS program, and consistently fitted using PyORBIT. We derived RV detection maps and calculated occurrence rates for ISPs, cross-validating results with two independent codes. The sample was divided into subgroups to evaluate how system parameters influence planet occurrence. Results. We confirmed the 213 already known planets in the 137 systems and also identified six new candidates. We divided them, based on mass and period, into Neptunes (10 < m sin i < 31.7 M$_{\oplus}$) and Super-Earths (3 < m sin i < 10 M$_{\oplus}$), and into hot (1 < P < 10 d), warm (10 < P < 100 d), and cool (100 < P < 400 d). We found occurrences of 5%, 13%, and 12% for hot, warm, and cool Neptunes, respectively, and 11% and 16% for hot and warm Super-Earths, respectively. Systems with dynamically stable inner regions show higher rates of small planets. These findings are consistent with previous studies showing no strong correlation between ISPs and CJs at average stellar metallicity and mass, and suggest that HJs may be more commonly associated with external giants.
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Reviewed July 14, 2026 · model on record in the stance chip above.
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