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Cold Jupiters and small planets: Friends, foes, or indifferent? A search for correlations with the largest exoplanet samples

T0 review · 2 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Cold Jupiters and small planets are mostly unrelated, census shows

desk verdict A careful, larger-sample recomputation that settles the cold-Jupiter occurrence rate around small-planet hosts near ~11%, with a plausible but sub-3-sigma excess at super-solar mass/metallicity and an under-powered eccentricity-multiplicity trend. read the letter →

arxiv 2505.20035 v2 pith:N23VSTWX submitted 2025-05-26 astro-ph.EP astro-ph.SR

A. S. Bonomo , L. Naponiello , E. Pezzetta , A. Sozzetti , D. Gandolfi , R. Wittenmyer , M. Pinamonti This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords coldJupiterssmallplanetsexoplanetoccurrenceratesplanetformationradialvelocitysurveysstellarmetallicityplanetarysystemarchitecturedemographics
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Does a star's short-period small planets tell you anything about whether it also hosts a distant cold Jupiter? This paper answers with a large homogeneous comparison: the cold-Jupiter rate in 217 small-planet systems is $f_{\rm CJ|SP}=11.1^{+2.5}_{-1.8}\%$, statistically the same as the $9.8^{+0.9}_{-0.8}\%$ rate measured in a comparison sample of 1167 solar-type stars from blind radial-velocity surveys. The only deviation appears in stars with super-solar mass and metallicity, where the rate is higher but the excess is below $3\sigma$. The authors conclude that small planets and cold Jupiters are mostly indifferent to each other, with a possible exception in massive metal-rich stars, and that the two populations' occurrence rates cannot be used to argue for strong formation coupling.

What carries the argument

The analysis rests on paired samples and a per-star completeness correction. The small-planet sample is drawn from public catalogs using fixed criteria (confirmed planet mass, solar-type host, public radial velocities with more than 20 epochs spanning at least one year), and the comparison sample is a merged set of stars from three large radial-velocity surveys selected under the same stellar criteria. For each star, the sensitivity to cold Jupiters is computed by injecting synthetic Keplerian signals on a $30\times30$ grid in planet mass and semimajor axis, drawing eccentricities from a $\beta$ distribution, and counting recoveries with a model-selection criterion; the average recovery rate converts the raw star count into an effective number of stars per bin. Occurrence rates are then derived from binomial statistics, and differences between rates are evaluated across metallicity and mass bins, with two-sample distribution tests used to check that the samples being compared are not too dissimilar.

What would settle it

A decisive test is to recompute $f_{\rm CJ|SP}$ using only systems in which the radial-velocity monitoring was planned without any prior hint of an outer companion—for example, targets selected purely by transit detection. If the rate in that unbiased subsample matches $f_{\rm CJ}$ in every mass-metallicity bin, the tentative super-solar excess is a selection artifact; if it exceeds $f_{\rm CJ}$ at super-solar mass and metallicity at more than $3\sigma$, the correlation is real.

Watch

Extended reading notes

Core claim

On its own terms, the paper's discovery is that the occurrence of cold Jupiters does not depend on whether a system also has short-period small planets, once selection effects are handled homogeneously. Using 217 systems with confirmed small planets and a merged comparison sample of 1167 stars from three radial-velocity surveys, it obtains an integrated rate $f_{\rm CJ|SP}=11.1^{+2.5}_{-1.8}\%$ at average stellar metallicity and mass, fully consistent with $f_{\rm CJ}=9.8^{+0.9}_{-0.8}\%$ in the comparison sample. Broken down by stellar mass and metallicity, only the bin with $M_\star\ge1.0\,M_\odot$ and $[\mathrm{Fe/H}]>0.1$ shows an excess of cold Jupiters in small-planet systems, at $2.5\sigma$ for the $0.5$--$20\,M_{\rm Jup}$ mass range. The paper further finds no correlation with small-planet multiplicity, cold-Jupiter multiplicity, or small-planet composition, but does find that the multiplicity of inner small planets drops when the cold Jupiter is eccentric, as dynamical theory predicts.

Load-bearing premise

The load-bearing premise is that the 217 small-planet systems are representative of all small-planet systems, with no bias toward stars already known or suspected to host an outer cold Jupiter; if the sample is biased that way, the measured $11.1\%$ rate is inflated and the comparison against blind surveys is unfair.

Editorial extensions

If this is right

  • The previously reported $\sim40\%$ occurrence of cold Jupiters in small-planet systems is not reproduced; the new integrated rate is $11.1^{+2.5}_{-1.8}\%$.
  • Any SP-CJ correlation, if real, is confined to super-solar mass and metallicity and is currently below $3\sigma$; the default conclusion is that the two populations form independently.
  • The absence of SP-CJ trends with small-planet multiplicity, cold-Jupiter multiplicity, and small-planet composition weakens anticorrelation models in which cold Jupiters block the inward migration or growth of small planets.
  • The strong drop in inner-planet multiplicity around eccentric cold Jupiters means that even at equal occurrence rates, the architecture of a small-planet system is shaped by its outer giant.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If future larger samples confirm the indifference, formation models that predict a strong dynamical coupling between inner small planets and outer giants—such as the pebble-isolation barrier—would need to be revised or restricted to specific disk conditions.
  • A testable extension the authors do not pursue: apply the same completeness machinery to finer composition classes (rocky with thin envelopes versus water worlds), since the bulk-density degeneracy they note could hide an architecture-composition link.
  • The current $11.1\%$ rate is a lower bound in practice: the analysis counts only confirmed cold Jupiters, and three short-baseline small-planet systems show long-term radial-velocity trends that could turn out to be cold Jupiters; if so, the integrated rate would rise.
  • The tentative super-solar excess predicts that a future sample restricted to $M_\star>1.0\,M_\odot$ and $[\mathrm{Fe/H}]>0.1$ will show $f_{\rm CJ|SP}$ rising with metallicity; if it stays flat, the excess was a fluctuation.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The paper measures the occurrence rate of cold Jupiters (CJs, a=1-10 AU, M=0.5-20 MJup) around solar-type stars that host short-period small planets (SPs, P<100 d, 1-20 MEarth), using a sample of 217 SP systems with public RV data and a comparison sample of 1167 stars from the AAT, CLS, and HARPS surveys. Using binomial statistics with injection-recovery completeness, the authors find f_CJ|SP = 11.1^{+2.5}_{-1.8}%, consistent with f_CJ = 9.8^{+0.9}_{-0.8}%, and a possible excess only at super-solar mass and metallicity (2.5sigma). They also find no correlations with SP multiplicity, CJ multiplicity, or SP composition, but report that SP multiplicity is lower around eccentric CJs. The paper concludes that SPs and CJs are mostly independent, with a possible exception in massive metal-rich stars.

Significance. If correct, this is the largest homogeneous comparison to date of CJ occurrence in SP and non-SP hosts, and it strengthens the case that inner small planets and outer giants form largely independently. The use of three blind RV surveys merged into one sample, the consistent application of completeness corrections, and the public data make the analysis reproducible. However, the central comparison is threatened by a selection effect in the SP sample, which the paper does not quantify; the claimed super-solar correlation in particular rests on this assumption.

major comments (2)
  1. [§2.1, §2.3, §4.3, Table D.2] The SP sample selection in §2.1 requires at least one public RV dataset with more than 20 measurements and baseline ≥ 1 yr. This criterion is not selection-neutral: for transit-discovered SPs, extended RV monitoring is often triggered by suspected outer companions or RV trends, so systems with CJs are more likely to satisfy the criterion. The K-S tests in §2.3 compare stellar metallicity and mass distributions between the SP and comparison samples, but they do not address this target-selection effect. If the bias is present, f_CJ|SP is inflated, and the 2.5σ excess at super-solar mass and metallicity reported in §4.3 (Table D.2) could be entirely spurious. The authors should demonstrate that the SP sample is representative by, e.g., comparing f_CJ|SP between transit-detected SP systems with and without the required RV data, or by explicitly modeling the probability of having such data as a function of known companion status.
  2. [§2.3, §4.3, Table D.2] The comparison in §4.3 is made without matching the stellar parameter distributions of the SP and merged RV samples. Section 2.3 reports a K-S p-value of 3e-9 for stellar mass and p<0.01 for metallicity within the 1.0-1.2 Msun bin, indicating that the two samples are not drawn from similar parent distributions. Because f_CJ increases with both stellar mass and metallicity, the higher f_CJ|SP in the super-solar mass and metallicity bin could reflect these distributional differences rather than a genuine SP-CJ correlation. The paper should either reweight the comparison sample to match the SP sample's stellar parameter distribution or restrict the comparison to a matched subsample, and report the mean [Fe/H] and M_star within each bin to allow the reader to assess this.
minor comments (5)
  1. [§2.2] The description of the merged comparison sample says '1167 stars, 213 of which are common to two or all three surveys'; the paper should state explicitly whether the merged sample is the union of unique stars and whether each star is counted once in the binomial statistics, since double-counting common stars would distort the effective sample size.
  2. [§3, Eq. (1)] The binomial formula uses N_star,eff = N_star * C with an average completeness; this ignores the star-to-star variance in completeness, and the authors should comment on whether a hierarchical treatment would change the quoted uncertainties.
  3. [§4.2] The manuscript quotes a 1.7σ significance for the difference between f_CJ|SP and f_CJ at super-solar metallicity, but it does not specify how the significance was computed; please state the test statistic (e.g., a two-proportion z-test or a bootstrap).
  4. [Figure B.1] The color bars are difficult to read in the printed version; please increase the font size or adjust the layout so that the completeness scale is legible.
  5. [§5.2] The caveat that completeness values are optimistic because they ignore uncorrelated jitter is useful, but a quantitative estimate of the typical jitter effect on f_CJ would help the reader gauge the impact.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the occurrence rates are direct binomial estimates from target and comparison samples, not outputs of a model that assumes the result.

full rationale

The paper's central quantities, f_CJ|SP and f_CJ, are computed from the observed number of systems with cold Jupiters (d), the effective number of stars (N_star,eff), and an injection-recovery completeness correction, via the binomial likelihood in Eq. (1). These are measurements from the SP and RV comparison samples, not parameters fitted to produce the claimed agreement. The completeness methodology is borrowed from B23 and BL24, but that is a shared measurement technique, not a self-citation that supplies the conclusion; the paper independently recomputes completeness for its own samples and checks agreement with BL24. The comparison between f_CJ|SP = 11.1% and f_CJ = 9.8% is made after both quantities are estimated, so the consistency is not forced by construction. The marginal super-solar mass/metallicity excess is extracted from the same measured rates and is explicitly reported at below 3 sigma, with the small-number and selection caveats acknowledged. The conditional probability f_SP|CJ = f_SP * f_CJ|SP / f_CJ is an algebraic identity relating separately estimated rates, not a circular derivation. Potential selection bias in the SP sample definition (Sect. 2.1) is a legitimate correctness concern about representativeness, but it is not a form of circularity: the paper does not define the occurrence rate in terms of the conclusion, nor does any equation reduce to its own input. Therefore no circular step can be identified with the required specificity.

Assumptions & free parameters 0 free parameters · 5 assumptions · 0 invented entities

The analysis does not fit model parameters to data; it measures occurrence rates using binomial statistics with completeness corrections. The main assumptions are the representativeness of the comparison RV surveys, the validity of the completeness simulation (including its eccentricity prior and neglect of jitter), and the accuracy of stellar parameters from the Hypatia catalog. These are domain assumptions, not free parameters.

assumptions (5)
  • standard math Binomial statistics with effective star counts N_eff = N_star * C (Eq. 1)
    Used to compute occurrence rates and confidence intervals in Section 3.
  • domain assumption Eccentricity distribution of simulated CJs follows a Beta distribution from Kipping 2013
    Injection-recovery completeness in Section 3 assumes this eccentricity prior; if the true eccentricity distribution differs, completeness estimates change.
  • domain assumption Formal RV uncertainties, not stellar jitter, are used in completeness simulations
    Section 5.2 acknowledges completeness values are optimistic and assumes the effect is similar for SP and comparison samples.
  • domain assumption The AAT, CLS, and HARPS surveys, after applying selection criteria, provide an unbiased comparison sample for f_CJ
    Section 2.2 defines the comparison sample; if these surveys are not representative of the same stellar population as SP hosts, the comparison f_CJ is biased.
  • domain assumption Stellar masses and metallicities from the Hypatia catalog are accurate for binning
    Binning in Sections 3 and 4 relies on Hypatia catalog values; typical uncertainties of 0.04 to 0.07 dex are acknowledged.

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Cite this review

Pith. "Pith review of Cold Jupiters and small planets: Friends, foes, or indifferent? A search for correlations with the largest exoplanet samples." pith.science (2026). https://pith.science/paper/N23VSTWX

@misc{pith2026250520035,
  author       = {Pith},
  title        = {Pith review of: Cold Jupiters and small planets: Friends, foes, or indifferent? A search for correlations with the largest exoplanet samples},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/N23VSTWX}},
  note         = {Machine review of arXiv:2505.20035}
}
abstract

Determining whether there is any correlation between the presence of short-period small planets (SPs) with $P\lesssim100~d$ ($a \lesssim0.4~AU$) and $1<M_{p}<20~M_\oplus$ and that of outer cold Jupiters (CJs) with $a=1-10~AU$ and $M_{p}=0.5-20~M_{Jup}$ around solar-type stars may provide crucial constraints on models of formation and/or migration of SPs. However, discrepant results regarding the occurrence rates of CJs in SP systems have been reported in the literature, with some recent studies suggesting a strong SP-CJ correlation but only at super-solar metallicities and/or masses of the host stars. Here, we homogeneously recomputed the occurrence rates of CJs at average, sub-solar ($[Fe/H]<-0.1$), solar ($-0.1\le[Fe/H]\le0.1$), and super-solar ($[Fe/H]>0.1$) metallicity as well as at average and subintervals of stellar mass, namely 0.6-0.8, 0.8-1.0, and 1.0-1.2 $M_\odot$, using (i) a carefully-selected sample of 217 SP systems, and (ii) a large comparison sample of 1167 solar-type stars. We determine the integrated occurrence rate of CJs in SP systems to be $f_{CJ|SP}=11.1^{+2.5}_{-1.8}\%$; this is consistent with the estimated frequencies of CJs in both the comparison sample ($f_{CJ}=9.8^{+0.9}_{-0.8}\%$) and the HARPS-N survey of transiting SP systems. We find a possible correlation ($f_{CJ|SP}>f_{CJ}$) only at super-solar mass and metallicity, though with statistical confidence of less than $3\sigma$. To test some theoretical predictions, we also searched for possible SP-CJ relations as a function of SP and CJ multiplicity, as well as SP composition, and we found none. We show that the architectures of SP systems are not indifferent to the presence of CJs, because the multiplicity of SPs strongly depends on the CJ eccentricity, as expected from planetary dynamics. A more comprehensive understanding of the relation between SPs and CJs requires larger samples of SP systems.[Abridged]

Figures

Figures reproduced from arXiv: 2505.20035 by the authors.

Figure 1
Figure 1. Occurrence rates of CJs with Mp = 0.5 − 20 MJup in the SP sample (red solid line) and the merged RV comparison sample (black dashed line) at sub-solar ([Fe/H] < −0.1), solar (−0.1 ≤ [Fe/H] ≤ 0.1), and super-solar ([Fe/H] > 0.1) metallicity. See Table D.1. 4.2. Frequency of CJs as a function of stellar metallicity We report fCJ|SP and fCJ for the three subintervals of stellar metallicity (Sect. 3) in Table D.1and dis… view at source ↗
Figure 2
Figure 2. Same as [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Architectures of 27 systems with both SPs and CJs in the mass range 0.3 ≤ Mp ≤ 13 MJup, ordered according to increasing orbital ec￾centricity of the CJs (from top to bottom; for multiple CJs, the highest eccentricity is considered). The planet circles have sizes proportional to their mass (see legend in the top right corner), and colors indicating orbital eccentricity (more eccentric planets are shown in yellow). Ho… view at source ↗

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Forward citations

Cited by 3 Pith papers

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    astro-ph.EP 2026-07 accept novelty 6.0 of 10

    Occurrence rates of hot/warm/cool Neptunes and Super-Earths around cold-Jupiter hosts are ~5–16%, higher when the outer giant leaves a stable inner zone, with no strong ISP–CJ correlation at average metallicity.

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Works this paper leans on

183 extracted references · 67 canonical work pages · cited by 3 Pith papers

  1. [1]

    M., et al

    Ahrer , E., Queloz , D., Rajpaul , V. M., et al. 2021, , 503, 1248

    2021

  2. [2]

    M., Batalha , N

    Akana Murphy , J. M., Batalha , N. M., Scarsdale , N., et al. 2023, , 166, 153

    2023

  3. [3]

    M., Kosiarek , M

    Akana Murphy , J. M., Kosiarek , M. R., Batalha , N. M., et al. 2021, , 162, 294

    2021

  4. [4]

    2014, , 567, A112

    Alonso , R., Moutou , C., Endl , M., et al. 2014, , 567, A112

    2014

  5. [5]

    M., et al

    Alqasim , A., Grieves , N., Ros \'a rio , N. M., et al. 2024, , 533, 1

    2024

  6. [6]

    R., Collier Cameron , A., Delrez , L., et al

    Anderson , D. R., Collier Cameron , A., Delrez , L., et al. 2014, , 445, 1114

    2014

  7. [7]

    X., et al

    Astudillo-Defru , N., Cloutier , R., Wang , S. X., et al. 2020, , 636, A58

    2020

  8. [8]

    2017, , 602, A88

    Astudillo-Defru , N., Forveille , T., Bonfils , X., et al. 2017, , 602, A88

    2017

Show all 183 references
  1. [9]

    Azevedo Silva , T., Demangeon , O. D. S., Barros , S. C. C., et al. 2022, , 657, A68

    2022

  2. [10]

    2020, , 641, A68

    Barbato , D., Pinamonti , M., Sozzetti , A., et al. 2020, , 641, A68

    2020

  3. [11]

    2018, , 615, A175

    Barbato , D., Sozzetti , A., Desidera , S., et al. 2018, , 615, A175

    2018

  4. [12]

    C., Faherty , J

    Bardalez Gagliuffi , D. C., Faherty , J. K., Li , Y., et al. 2021, , 922, L43

    2021

  5. [13]

    R., Standing , M

    Barnes , J. R., Standing , M. R., Haswell , C. A., et al. 2023, , 524, 5196

    2023

  6. [14]

    Barros, S. C. C., Demangeon, O. D. S., Alibert, Y., et al. 2022, , 665, A154

    2022

  7. [15]

    Barros , S. C. C., Demangeon , O. D. S., Armstrong , D. J., et al. 2023, , 673, A4

    2023

  8. [16]

    A., Badnell , H., Blacker , S., & Triaud , A

    Baycroft , T. A., Badnell , H., Blacker , S., & Triaud , A. H. M. J. 2023, Research Notes of the American Astronomical Society, 7, 175

    2023

  9. [17]

    2024, , 167, 70

    Beard , C., Robertson , P., Dai , F., et al. 2024, , 167, 70

    2024

  10. [18]

    Benedict , G. F. & Harrison , T. E. 2017, , 153, 258

    2017

  11. [19]

    F., McArthur , B

    Benedict , G. F., McArthur , B. E., Nelan , E. P., et al. 2022, , 163, 295

    2022

  12. [20]

    & Izidoro , A

    Bitsch , B. & Izidoro , A. 2023, , 674, A178

    2023

  13. [21]

    S., Dumusque , X., Massa , A., et al

    Bonomo , A. S., Dumusque , X., Massa , A., et al. 2023, , 677, A33

    2023

  14. [22]

    S., Sozzetti , A., Lovis , C., et al

    Bonomo , A. S., Sozzetti , A., Lovis , C., et al. 2014, , 572, A2

    2014

  15. [23]

    M., Meunier , N., & Galland , F

    Borgniet , S., Lagrange , A. M., Meunier , N., & Galland , F. 2017, , 599, A57

    2017

  16. [24]

    J., Koch , D

    Borucki , W. J., Koch , D. G., Batalha , N., et al. 2012, , 745, 120

    2012

  17. [25]

    2018, , 619, A1

    Bourrier , V., Dumusque , X., Dorn , C., et al. 2018, , 619, A1

    2018

  18. [26]

    M., Zhao , L

    Brewer , J. M., Zhao , L. L., Fischer , D. A., et al. 2023, , 166, 46

    2023

  19. [27]

    L., Weiss , L

    Brinkman , C. L., Weiss , L. M., Dai , F., et al. 2023, , 165, 88

    2023

  20. [28]

    L., Knutson , H

    Bryan , M. L., Knutson , H. A., Lee , E. J., et al. 2019, , 157, 52

    2019

  21. [29]

    Bryan , M. L. & Lee , E. J. 2024, , 968, L25

    2024

  22. [30]

    Bryan , M. L. & Lee , E. J. 2025, , 982, L7

    2025

  23. [31]

    2021, , 161, 10

    Burt , J., Feng , F., Holden , B., et al. 2021, , 161, 10

    2021

  24. [32]

    P., Wright , J

    Butler , R. P., Wright , J. T., Marcy , G. W., et al. 2006, , 646, 505

    2006

  25. [33]

    E., Irwin , J., et al

    Cloutier , R., Rodriguez , J. E., Irwin , J., et al. 2020, , 160, 22

    2020

  26. [34]

    D., Fabrycky , D

    Cochran , W. D., Fabrycky , D. C., Torres , G., et al. 2011, , 197, 7

    2011

  27. [35]

    2015, , 581, A38

    Courcol , B., Bouchy , F., Pepe , F., et al. 2015, , 581, A38

    2015

  28. [36]

    W., Batalha , N

    Dai , F., Howard , A. W., Batalha , N. M., et al. 2021, , 162, 62

    2021

  29. [37]

    2024, , 531, 4464

    Dalal , S., Rescigno , F., Cretignier , M., et al. 2024, , 531, 4464

    2024

  30. [38]

    2023, , 679, A33

    Damasso , M., Rodrigues , J., Castro-Gonz \'a lez , A., et al. 2023, , 679, A33

    2023

  31. [39]

    Dawson , R. I. & Johnson , J. A. 2018, , 56, 175

    2018

  32. [40]

    J., Georgieva , I

    Deeg , H. J., Georgieva , I. Y., Nowak , G., et al. 2023, , 677, A12

    2023

  33. [41]

    2021, Nature Astronomy, 5, 775

    Delrez , L., Ehrenreich , D., Alibert , Y., et al. 2021, Nature Astronomy, 5, 775

    2021

  34. [42]

    V., Harada , C

    Desai , A., Turtelboom , E. V., Harada , C. K., et al. 2024, , 167, 194

    2024

  35. [43]

    F., S \'e gransan , D., Udry , S., et al

    D \' az , R. F., S \'e gransan , D., Udry , S., et al. 2016, , 585, A134

    2016

  36. [44]

    2023, , 165, 38

    DiTomasso , V., Nava , C., L \'o pez-Morales , M., et al. 2023, , 165, 38

    2023

  37. [45]

    F., Cristofari , P

    Donati , J. F., Cristofari , P. I., Finociety , B., et al. 2023, , 525, 455

    2023

  38. [46]

    2019, , 627, A43

    Dumusque , X., Turner , O., Dorn , C., et al. 2019, , 627, A43

    2019

  39. [47]

    A., Horner , J., et al

    Errico , A., Wittenmyer , R. A., Horner , J., et al. 2022, , 163, 273

    2022

  40. [48]

    P., Vogt , S

    Feng , F., Butler , R. P., Vogt , S. S., et al. 2022, , 262, 21

    2022

  41. [49]

    D., Xuesong Wang , S., et al

    Feng , F., Crane , J. D., Xuesong Wang , S., et al. 2019, , 242, 25

    2019

  42. [50]

    A., Clement , M

    Feng , F., Shectman , S. A., Clement , M. S., et al. 2020, , 250, 29

    2020

  43. [51]

    Feng , F., Tuomi , M., & Jones , H. R. A. 2017, , 470, 4794

    2017

  44. [52]

    A., Gaidos , E., Howard , A

    Fischer , D. A., Gaidos , E., Howard , A. W., et al. 2012, , 745, 21

    2012

  45. [53]

    Fischer , D. A. & Valenti , J. 2005, , 622, 1102

    2005

  46. [54]

    Frensch , Y. G. C., Lo Curto , G., Bouchy , F., et al. 2023, , 675, A173

    2023

  47. [55]

    Fulton , B. J. & Petigura , E. A. 2018, , 156, 264

    2018

  48. [56]

    J., Rosenthal , L

    Fulton , B. J., Rosenthal , L. J., Hirsch , L. A., et al. 2021, , 255, 14

    2021

  49. [57]

    X., et al

    Gan , T., Bedell , M., Wang , S. X., et al. 2021, , 507, 2220

    2021

  50. [58]

    E., & Sari , R

    Ginzburg , S., Schlichting , H. E., & Sari , R. 2018, , 476, 759

    2018

  51. [59]

    K., Saunders , N., Huber , D., et al

    Grunblatt , S. K., Saunders , N., Huber , D., et al. 2024, , 168, 1

    2024

  52. [60]

    P., Rivera , E

    Haghighipour , N., Butler , R. P., Rivera , E. J., Henry , G. W., & Vogt , S. S. 2012, , 756, 91

    2012

  53. [61]

    C., Bouchy , F., Stalport , M., et al

    Hara , N. C., Bouchy , F., Stalport , M., et al. 2020, , 636, L6

    2020

  54. [62]

    P., Gandolfi , D., Korth , J., et al

    Hatzes , A. P., Gandolfi , D., Korth , J., et al. 2022, , 163, 223

    2022

  55. [63]

    G., et al

    Hawthorn , F., Bayliss , D., Wilson , T. G., et al. 2023, , 520, 3649

    2023

  56. [64]

    D., Collier Cameron , A., Queloz , D., et al

    Haywood , R. D., Collier Cameron , A., Queloz , D., et al. 2014, , 443, 2517

    2014

  57. [65]

    2010, , 512, A46

    H \'e brard , G., Udry , S., Lo Curto , G., et al. 2010, , 512, A46

    2010

  58. [66]

    2022, , 658, A176

    Heidari , N., Boisse , I., Orell-Miquel , J., et al. 2022, , 658, A176

    2022

  59. [67]

    2020, , 636, A89

    Hidalgo , D., Pall \'e , E., Alonso , R., et al. 2020, , 636, A89

    2020

  60. [68]

    R., Timmes , F

    Hinkel , N. R., Timmes , F. X., Young , P. A., Pagano , M. D., & Turnbull , M. C. 2014, , 148, 54

    2014

  61. [69]

    J., Bouchy , F., Lavie , B., et al

    Hobson , M. J., Bouchy , F., Lavie , B., et al. 2024, , 688, A216

    2024

  62. [70]

    J., D \' az , R

    Hobson , M. J., D \' az , R. F., Delfosse , X., et al. 2018, , 618, A103

    2018

  63. [71]

    2023, , 674, A10

    Holl , B., Sozzetti , A., Sahlmann , J., et al. 2023, , 674, A10

    2023

  64. [72]

    A., Wright , D

    Horner , J., Wittenmyer , R. A., Wright , D. J., et al. 2019, , 158, 100

    2019

  65. [73]

    X., Teske , J

    Hua , X., Wang , S. X., Teske , J. K., et al. 2023, , 166, 32

    2023

  66. [74]

    X., Petrovich , C., & Deibert , E

    Huang , C. X., Petrovich , C., & Deibert , E. 2017, , 153, 210

    2017

  67. [75]

    N., Morbidelli , A., Hersant , F., & Pierens , A

    Izidoro , A., Raymond , S. N., Morbidelli , A., Hersant , F., & Pierens , A. 2015, , 800, L22

    2015

  68. [76]

    S., Jones , H

    Jenkins , J. S., Jones , H. R. A., Tuomi , M., et al. 2017, , 466, 443

    2017

  69. [77]

    S., Jones , H

    Jenkins , J. S., Jones , H. R. A., Tuomi , M., et al. 2013, , 766, 67

    2013

  70. [78]

    A., Aller , K

    Johnson , J. A., Aller , K. M., Howard , A. W., & Crepp , J. R. 2010, , 122, 905

    2010

  71. [79]

    R., Yal c nkaya , S., Osborn , H

    Kane , S. R., Yal c nkaya , S., Osborn , H. P., et al. 2020, , 160, 129

    2020

  72. [80]

    2022, , 657, A7

    Kervella , P., Arenou , F., & Th \'e venin , F. 2022, , 657, A7

    2022

  73. [81]

    Kipping , D. M. 2013, , 434, L51

    2013

  74. [82]

    2024, , 971, L28

    Korth , J., Chaturvedi , P., Parviainen , H., et al. 2024, , 971, L28

    2024

  75. [83]

    X., et al

    Kunimoto , M., Vanderburg , A., Huang , C. X., et al. 2023, , 166, 7

    2023

  76. [84]

    Lam , K. W. F., Santerne , A., Sousa , S. G., et al. 2018, , 620, A77

    2018

  77. [85]

    A., et al

    Lambrechts , M., Morbidelli , A., Jacobson , S. A., et al. 2019, , 627, A83

    2019

  78. [86]

    R., Brandt , T

    Li , Z., Kane , S. R., Brandt , T. D., et al. 2024, , 167, 155

    2024

  79. [87]

    P., Su \'a rez Mascare \ n o , A., et al

    Lillo-Box , J., Faria , J. P., Su \'a rez Mascare \ n o , A., et al. 2021, , 654, A60

    2021

  80. [88]

    A., Santerne , A., et al

    Lillo-Box , J., Lopez , T. A., Santerne , A., et al. 2020, , 640, A48

    2020

  81. [89]

    2013, , 551, A59

    Lo Curto , G., Mayor , M., Benz , W., et al. 2013, , 551, A59

    2013

  82. [90]

    2010, , 512, A48

    Lo Curto , G., Mayor , M., Benz , W., et al. 2010, , 512, A48

    2010

  83. [91]

    Lopez , E. D. & Fortney , J. J. 2014, , 792, 1

    2014

  84. [92]

    2011, , 528, A112

    Lovis , C., S \'e gransan , D., Mayor , M., et al. 2011, , 528, A112

    2011

  85. [93]

    2022, , 163, 101

    Lubin , J., Van Zandt , J., Holcomb , R., et al. 2022, , 163, 101

    2022

  86. [94]

    K., Bastien , F

    Luhn , J. K., Bastien , F. A., Wright , J. T., et al. 2019, , 157, 149

    2019

  87. [95]

    P., Leleu , A., et al

    Luque , R., Osborn , H. P., Leleu , A., et al. 2023, , 623, 932

    2023

  88. [96]

    G., Petigura , E

    MacDougall , M. G., Petigura , E. A., Fetherolf , T., et al. 2022, , 164, 97

    2022

  89. [97]

    G., Petigura , E

    MacDougall , M. G., Petigura , E. A., Gilbert , G. J., et al. 2023, , 166, 33

    2023

  90. [98]

    2024, , 682, A129

    Mantovan , G., Malavolta , L., Desidera , S., et al. 2024, , 682, A129

    2024

  91. [99]

    W., Isaacson , H., Howard , A

    Marcy , G. W., Isaacson , H., Howard , A. W., et al. 2014, , 210, 20

    2014

  92. [100]

    2013, , 551, A90

    Marmier , M., S \'e gransan , D., Udry , S., et al. 2013, , 551, A90

    2013

  93. [101]

    2023, , 680, A84

    Martioli , E., H \'e brard , G., de Almeida , L., et al. 2023, , 680, A84

    2023

  94. [102]

    2022, , 660, A86

    Martioli , E., H \'e brard , G., Fouqu \'e , P., et al. 2022, , 660, A86

    2022

  95. [103]

    2023, , 677, A133

    Matuszewski , F., Nettelmann , N., Cabrera , J., B \"o rner , A., & Rauer , H. 2023, , 677, A133

    2023

  96. [104]

    W., Dressing , C

    Mayo , A. W., Dressing , C. D., Vanderburg , A., et al. 2023, , 165, 235

    2023

  97. [105]

    2011, arXiv e-prints, arXiv:1109.2497

    Mayor , M., Marmier , M., Lovis , C., et al. 2011, arXiv e-prints, arXiv:1109.2497

    2011 arXiv

  98. [106]

    P., Tinney , C

    McCarthy , C., Butler , R. P., Tinney , C. G., et al. 2004, , 617, 575

    2004

  99. [107]

    A., Bakos , G., Howard , A

    Ment , K., Fischer , D. A., Bakos , G., Howard , A. W., & Isaacson , H. 2018, , 156, 213

    2018

  100. [108]

    P., Santos , N

    Mortier , A., Faria , J. P., Santos , N. C., et al. 2016, , 585, A135

    2016

  101. [109]

    C., Sousa , S., et al

    Mortier , A., Santos , N. C., Sousa , S., et al. 2013, , 551, A112

    2013

  102. [110]

    M., D \' az , R

    Moutou , C., Almenara , J. M., D \' az , R. F., et al. 2014, , 444, 2783

    2014

  103. [111]

    2015, , 576, A48

    Moutou , C., Lo Curto , G., Mayor , M., et al. 2015, , 576, A48

    2015

  104. [112]

    2009, , 496, 513

    Moutou , C., Mayor , M., Lo Curto , G., et al. 2009, , 496, 513

    2009

  105. [113]

    2007, , 470, 721

    Naef , D., Mayor , M., Benz , W., et al. 2007, , 470, 721

    2007

  106. [114]

    2010, , 523, A15

    Naef , D., Mayor , M., Lo Curto , G., et al. 2010, , 523, A15

    2010

  107. [115]

    2022, , 667, A8

    Naponiello , L., Mancini , L., Damasso , M., et al. 2022, , 667, A8

    2022

  108. [116]

    2023, , 622, 255

    Naponiello , L., Mancini , L., Sozzetti , A., et al. 2023, , 622, 255

    2023

  109. [117]

    in prep.,

    Naponiello, L., et al. in prep.,

  110. [118]

    2022, , 664, A163

    Nardiello , D., Malavolta , L., Desidera , S., et al. 2022, , 664, A163

    2022

  111. [119]

    2023, , 673, A42

    Nascimbeni , V., Borsato , L., Zingales , T., et al. 2023, , 673, A42

    2023

  112. [120]

    2024, , 684, A96

    Orell-Miquel , J., Carleo , I., Murgas , F., et al. 2024, , 684, A96

    2024

  113. [121]

    2023, , 669, A40

    Orell-Miquel , J., Nowak , G., Murgas , F., et al. 2023, , 669, A40

    2023

  114. [122]

    J., Cale , B., et al

    Osborn , A., Armstrong , D. J., Cale , B., et al. 2021, , 507, 2782

    2021

  115. [123]

    P., Nowak , G., H \'e brard , G., et al

    Osborn , H. P., Nowak , G., H \'e brard , G., et al. 2023, , 523, 3069

    2023

  116. [124]

    Osborne , H. L. M., Van Eylen , V., Goffo , E., et al. 2024, , 527, 11138

    2024

  117. [125]

    J., Montet , B

    Otor , O. J., Montet , B. T., Johnson , J. A., et al. 2016, , 152, 165

    2016

  118. [126]

    A., Mortier , A., et al

    Palethorpe , L., John , A. A., Mortier , A., et al. 2024, , 529, 3323

    2024

  119. [127]

    2017, , 608, A63

    Perger , M., Ribas , I., Damasso , M., et al. 2017, , 608, A63

    2017

  120. [128]

    A., Benneke , B., Batygin , K., et al

    Petigura , E. A., Benneke , B., Batygin , K., et al. 2018, , 156, 89

    2018

  121. [129]

    A., Livingston , J., Batygin , K., et al

    Petigura , E. A., Livingston , J., Batygin , K., et al. 2020, , 159, 2

    2020

  122. [130]

    A., Rogers , J

    Petigura , E. A., Rogers , J. G., Isaacson , H., et al. 2022, , 163, 179

    2022

  123. [131]

    M., Kiefer , F., et al

    Philipot , F., Lagrange , A. M., Kiefer , F., et al. 2023, , 678, A107

    2023

  124. [132]

    A., Kane, S

    Pidhorodetska, D., Gilbert, E. A., Kane, S. R., et al. 2024, , 168, 135

    2024

  125. [133]

    2022, , 664, A65

    Pinamonti , M., Sozzetti , A., Maldonado , J., et al. 2022, , 664, A65

    2022

  126. [134]

    S., Lubin , J., Beard , C., et al

    Polanski , A. S., Lubin , J., Beard , C., et al. 2024, , 272, 32

    2024

  127. [135]

    2024, , 685, A5

    Psaridi , A., Osborn , H., Bouchy , F., et al. 2024, , 685, A5

    2024

  128. [136]

    2025, Exp

    Rauer , H., Aerts , C., Cabrera , J., et al. 2025, Exp. Astron., 59, 26

    2025

  129. [137]

    2014, Exp

    Rauer , H., Catala , C., Aerts , C., et al. 2014, Exp. Astron., 38, 249

    2014

  130. [138]

    2024, , 527, 5385

    Rescigno , F., H \'e brard , G., Vanderburg , A., et al. 2024, , 527, 5385

    2024

  131. [139]

    L., S \'e gransan , D., Marmier , M., et al

    Rickman , E. L., S \'e gransan , D., Marmier , M., et al. 2019, , 625, A71

    2019

  132. [140]

    J., Fulton , B

    Rosenthal , L. J., Fulton , B. J., Hirsch , L. A., et al. 2021, , 255, 8

    2021

  133. [141]

    J., Knutson , H

    Rosenthal , L. J., Knutson , H. A., Chachan , Y., et al. 2022, , 262, 1

    2022

  134. [142]

    A., Dai , F., Howard , A

    Rubenzahl , R. A., Dai , F., Howard , A. W., et al. 2024, , 167, 153

    2024

  135. [143]

    in prep.,

    Ruggieri, A., et al. in prep.,

  136. [144]

    C., Santerne , A., Faria , J

    Santos , N. C., Santerne , A., Faria , J. P., et al. 2016, , 592, A13

    2016

  137. [145]

    2021, , 162, 215

    Scarsdale, N., Murphy, J., Batalha, N., et al. 2021, , 162, 215

    2021

  138. [146]

    2021, , 656, A71

    Schlecker , M., Mordasini , C., Emsenhuber , A., et al. 2021, , 656, A71

    2021

  139. [147]

    M., Gandolfi , D., Mustill , A

    Serrano , L. M., Gandolfi , D., Mustill , A. J., et al. 2022, Nature Astronomy, 6, 736

    2022

  140. [148]

    W., Petigura , E

    Sinukoff , E., Howard , A. W., Petigura , E. A., et al. 2017, , 153, 271

    2017

  141. [149]

    G., Santos , N

    Sousa , S. G., Santos , N. C., Israelian , G., Mayor , M., & Udry , S. 2011, , 533, A141

    2011

  142. [150]

    2024, Comptes Rendus Physique, 24, 152

    Sozzetti , A. 2024, Comptes Rendus Physique, 24, 152

    2024

  143. [151]

    S., et al

    Sozzetti , A., Damasso , M., Bonomo , A. S., et al. 2021, , 648, A75

    2021

  144. [152]

    2024, , 535, 531

    Sozzetti, A., Damasso, M., Fernández Fernández, J., et al. 2024, , 535, 531

    2024

  145. [153]

    R., Perdelwitz , V., Tal-Or , L., et al

    Sreenivas , K. R., Perdelwitz , V., Tal-Or , L., et al. 2022, , 660, A124

    2022

  146. [154]

    2023, , 678, A90

    Stalport , M., Cretignier , M., Udry , S., et al. 2023, , 678, A90

    2023

  147. [155]

    G., Collins , K

    Stassun , K. G., Collins , K. A., & Gaudi , B. S. 2017, , 153, 136

    2017

  148. [156]

    I., Rebolo , R., et al

    Su \'a rez Mascare \ n o , A., Gonz \'a lez Hern \'a ndez , J. I., Rebolo , R., et al. 2018, , 612, A41

    2018

  149. [157]

    M., Gonz \'a lez Hern \'a ndez , J

    Su \'a rez Mascare \ n o , A., Passegger , V. M., Gonz \'a lez Hern \'a ndez , J. I., et al. 2024, , 685, A56

    2024

  150. [158]

    Sulis , S., Crossfield , I. J. M., Santerne , A., et al. 2024, , 688, A14

    2024

  151. [159]

    R., Luque , R., et al

    Teske , J., D \' az , M. R., Luque , R., et al. 2020, , 160, 96

    2020

  152. [160]

    2020, , 636, A74

    Trifonov , T., Tal-Or , L., Zechmeister , M., et al. 2020, , 636, A74

    2020

  153. [161]

    Tuomi , M., Jones , H. R. A., Barnes , J. R., Anglada-Escud \'e , G., & Jenkins , J. S. 2014, , 441, 1545

    2014

  154. [162]

    V., Weiss , L

    Turtelboom , E. V., Weiss , L. M., Dressing , C. D., et al. 2022, , 163, 293

    2022

  155. [163]

    2019, , 622, A37

    Udry , S., Dumusque , X., Lovis , C., et al. 2019, , 622, A37

    2019

  156. [164]

    2021, , 654, A104

    Unger , N., S \'e gransan , D., Queloz , D., et al. 2021, , 654, A104

    2021

  157. [165]

    A., MacDougall , M., et al

    Van Zandt , J., Petigura , E. A., MacDougall , M., et al. 2023, , 165, 60

    2023

  158. [166]

    C., Buchhave , L

    Vanderburg , A., Becker , J. C., Buchhave , L. A., et al. 2017, , 154, 237

    2017

  159. [167]

    2020, , 159, 108

    Vissapragada , S., Jontof-Hutter , D., Shporer , A., et al. 2020, , 159, 108

    2020

  160. [168]

    S., Butler , R

    Vogt , S. S., Butler , R. P., Burt , J., et al. 2017, , 154, 181

    2017

  161. [169]

    M., Isaacson , H., Howard , A

    Weiss , L. M., Isaacson , H., Howard , A. W., et al. 2024, , 270, 8

    2024

  162. [170]

    A., Endl , M., Cochran , W

    Wittenmyer , R. A., Endl , M., Cochran , W. D., Levison , H. F., & Henry , G. W. 2009, , 182, 97

    2009

  163. [171]

    A., Horner , J., Mengel , M

    Wittenmyer , R. A., Horner , J., Mengel , M. W., et al. 2017, , 153, 167

    2017

  164. [172]

    A., Tan , X., Lee , M

    Wittenmyer , R. A., Tan , X., Lee , M. H., et al. 2014, , 780, 140

    2014

  165. [173]

    A., Wang , S., Horner , J., et al

    Wittenmyer , R. A., Wang , S., Horner , J., et al. 2020, , 492, 377

    2020

  166. [174]

    2023, Research in Astronomy and Astrophysics, 23, 055022

    Xiao , G.-Y., Liu , Y.-J., Teng , H.-Y., et al. 2023, Research in Astronomy and Astrophysics, 23, 055022

    2023

  167. [175]

    2009, , 505, 859–871

    Zechmeister, M., Kürster, M., & Endl, M. 2009, , 505, 859–871

    2009

  168. [176]

    & Sasselov , D

    Zeng , L. & Sasselov , D. 2013, , 125, 227

    2013

  169. [177]

    M., Huber, D., et al

    Zhang, J., Weiss, L. M., Huber, D., et al. 2021, , 162, 89

    2021

  170. [178]

    2024, Research in Astronomy and Astrophysics, 24, 045013

    Zhu , W. 2024, Research in Astronomy and Astrophysics, 24, 045013

    2024

  171. [179]

    & Dong , S

    Zhu , W. & Dong , S. 2021, , 59, 291

    2021

  172. [180]

    2018, , 860, 101

    Zhu , W., Petrovich , C., Wu , Y., Dong , S., & Xie , J. 2018, , 860, 101

    2018

  173. [181]

    & Wu , Y

    Zhu , W. & Wu , Y. 2018, , 156, 92

    2018

  174. [182]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sent...

  175. [183]

    write newline

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Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.