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Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396

T0 review · 2 major / 4 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The three-planet system TOI-396 has nearly equal planet radii, but the newly measured masses show the outermost planet is the densest, and the inner pair's transit-timing variations place it close to, but outside, the 5:3 mean-motion…

desk verdict Solid benchmark characterization of a bright multi-planet system; the new RV masses for b and d are probably right, with caveats on the eccentricity assumption and the TTV-derived mass of c. read the letter →

arxiv 2411.14911 v2 pith:MK7TUQSE submitted 2024-11-22 astro-ph.EP

A. Bonfanti , I. Amateis , D. Gandolfi , L. Borsato , J.A. Egger , P.E. Cubillos , D. Armstrong , I.C. Leão
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M. Fridlund B.L. Canto Martins S.G. Sousa J.R. De Medeiros L. Fossati V. Adibekyan A. Collier Cameron S. Grziwa K.W.F. Lam E. Goffo L.D. Nielsen F. Rodler J. Alarcon J. Lillo-Box W.D. Cochran R. Luque S. Redfield N.C. Santos S.C.C. Barros D. Bayliss X. Dumusque M.A.F. Keniger J. Livingston F. Murgas G. Nowak A. Osborn H.P. Osborn E. Pallé C.M. Persson L.M. Serrano P.A. Str{o}m S. Udry P.J. Wheatley
This is my paper · ORCID
classification astro-ph.EP
keywords TOI-396transit-timingvariationsmeanmotionresonanceradialvelocitiesstellaractivityplanetarymassesTESSphotometryHARPSspectroscopy
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

This paper establishes the architecture of TOI-396, the brightest known star hosting three transiting planets. Combining four TESS sectors with HARPS radial velocities, the authors refine the three radii to near-identical values around 2 Earth radii and, for the first time, measure Doppler masses for the inner and outer planets: TOI-396 b at 3.55 Earth masses and TOI-396 d at 7.1 Earth masses, making the outermost planet the densest. The middle planet, TOI-396 c, is invisible in the radial-velocity data because its 5.97-day orbit nearly coincides with the star's 6.7-day rotation period, but significant and anti-correlated transit-timing variations confirm its gravitational presence. A dynamical fit and a 10,000-year integration of the resonance angles show that planets b and c are close to, but not inside, the 5:3 mean-motion resonance. If these results hold, the system becomes a bright, nearby laboratory for testing how equal-size planets acquire very different densities.

What carries the argument

The argument is carried by a joint analysis of 41 TESS transit light curves and HARPS radial velocities in an MCMC framework, with stellar activity removed from the RVs by a breakpoint method that splits the time series at a statistically selected epoch and de-trends each segment separately. The resonance question is decided by the critical angles $\phi_b = 3\lambda_b - 5\lambda_c + 2\varpi_b$ and $\phi_c = 3\lambda_b - 5\lambda_c + 2\varpi_c$ of the 5:3 mean-motion resonance: if these angles librate the pair is trapped in resonance, and if they circulate it is not. An N-body dynamical fit to the RVs and transit times supplies the planet masses from the TTVs, while forward integrations predict how the transit-timing amplitudes grow with time.

What would settle it

Full TTV phase coverage over the predicted ~5-year super-period would settle the dynamical picture: if the transit times do not show the modeled drift of up to about 5 hours for b and 10 hours for c, or if a Keplerian signal near 5.97 days emerges in a longer activity-calibrated RV baseline, the paper's TTV solution and its explanation for the RV non-detection of planet c would be ruled out.

Watch

Extended reading notes

Core claim

On the paper's own terms, the central discovery is that the three TOI-396 planets have essentially equal radii—$R_b = 2.004^{+0.045}_{-0.047}\,R_\oplus$, $R_c = 1.979^{+0.054}_{-0.051}\,R_\oplus$, and $R_d = 2.001^{+0.063}_{-0.064}\,R_\oplus$—while their masses differ: the first RV-based mass determinations give $M_b = 3.55^{+0.94}_{-0.96}\,M_\oplus$ and $M_d = 7.1 \pm 1.6\,M_\oplus$, with bulk densities of $2.44$ and $4.9$ g cm$^{-3}$. The outermost planet being the densest is an unusual architecture. TOI-396 c remains undetected in the RVs, and the paper argues this is because its period is too close to the stellar rotation period; instead, its presence is established by significant, anticorrelated transit-timing variations in planets b and c. The dynamical analysis yields a formally precise mass for c of $M_{c,\mathrm{dyn}} = 2.24^{+0.13}_{-0.67}\,M_\oplus$, which the authors caution may be inaccurate until the TTV phase is fully sampled, and it shows the b–c pair is close to but out of the 5:3 mean-motion resonance.

Load-bearing premise

The load-bearing assumption is that all three planets follow circular orbits; if the near-resonant pair b and c has non-negligible eccentricity, the fitted radial-velocity amplitudes and thus the derived masses could be biased.

Editorial extensions

If this is right

  • If the architecture is real, TOI-396 joins the small set of systems where three similar-radius planets have resolved density differences, directly testing 'peas in a pod' formation models.
  • Future transit observations of planets b and c must account for predicted timing drifts of up to roughly 5 and 10 hours, respectively, relative to the linear ephemeris.
  • Completing the TTV phase coverage—for example with additional TESS or CHEOPS photometry—should turn the formal dynamical mass of planet c into a reliable one.
  • The injection tests imply that any planet with an orbital period near the stellar rotation period will have its RV signal systematically suppressed, so non-detections in such cases are not strong mass upper limits.
  • JWST eclipse observations with 2, 4, and 8 events for planets b, c, and d should distinguish primary from secondary atmospheres at the 3σ level, linking bulk density to atmospheric composition.

Reading between the lines

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

  • If the dynamical mass of planet c near 2.2 Earth masses survives full TTV sampling, the three planets would cover a factor-of-three mass range at nearly identical radii, making TOI-396 a sharper test of radius plateau models than a single-mass target.
  • The same activity-suppression effect demonstrated here may apply to other RV surveys: planets with periods within about one day of the stellar rotation period could be systematically missing from Doppler mass catalogs, biasing demographic conclusions.
  • A dedicated campaign spanning the predicted ~5-year TTV super-period could turn TOI-396 b and c into a precise dynamical clock, potentially revealing additional companions or tidal effects through deviations from the current N-body model.
  • The anti-correlated TTVs already provide an independent, photometric confirmation that planet c exists; this supports the use of TTVs as a discovery channel for planets hidden from RV surveys by activity.
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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 / 4 minor

Summary. The paper presents a joint analysis of TESS transit photometry and HARPS radial velocities of the bright F6V star TOI-396, which hosts three transiting planets near 2 Earth radii. Using MCMC joint fits with breakpoint-based activity detrending, the authors refine the planet radii (Rb=2.004+0.045-0.047, Rc=1.979+0.054-0.051, Rd=2.001+0.063-0.064 Rearth), report first RV mass detections for b (Mb=3.55+0.94-0.96 Mearth) and d (Md=7.1+/-1.6 Mearth), and a 3-sigma upper limit for c (Mup,c=3.8 Mearth). They identify significant TTVs for b and c with an anti-correlated pattern, perform a TRADES dynamical analysis yielding a formally precise but explicitly caveated mass for c (Mc,dyn=2.24+0.13-0.67 Mearth), find the b-c pair is near but not inside the 5:3 MMR, and forecast TTV amplitudes up to ~5 hours over a 5.2-year baseline. They also simulate JWST eclipse observations. The paper is transparent about the limitations of the TTV-derived mass and about the RV non-detection of c, attributing the latter to proximity of Pc to the stellar rotation period (Prot=6.7+/-1.3 d).

Significance. If the measured masses hold, the system is unusual in that the outermost planet is the densest, and the very bright host star (V~6.4) makes TOI-396 an important benchmark for formation models and JWST atmospheric characterization. The paper is methodologically careful in several respects: BIC-based model selection, breakpoint activity correction, explicit jitter modeling, MCMC convergence checks, injection-recovery tests for activity periods, and frank caveats about the TTV mass. The improved radii (~1.4x precision over Vanderburg et al. 2019) and the first RV masses for b and d are concrete contributions. However, the headline masses rest on a circular-orbit assumption whose evidential basis is weaker than the reported ΔBIC implies, and the stability of the small RV semi-amplitudes against the adopted eccentricity and activity model is not demonstrated. These points need to be addressed before the central mass claims can be considered robust.

major comments (2)
  1. [Section 4 and Table 2] The circular-orbit assumption is load-bearing for the headline masses (K_b=1.30+0.34-0.35 m/s and K_d=1.78+/-0.40 m/s are comparable to the 1.49 m/s jitter), but the evidence for e=0 is internally inconsistent. The paragraph that rejects eccentric orbits states both that the eccentric MCMC runs have "the poorer the parameter convergence" and that the data "are not enough to constrain the planetary eccentricities well," yet it then uses ΔBIC = BIC(e!=0)-BIC(e=0) ≳ +100 to discard them. For six additional parameters, a converged eccentric fit would carry a BIC penalty of only ~ln(N) per parameter (~26 for 78 RVs); a ΔBIC of +100 therefore implies either a large chi-square difference that is hard to believe given the stated convergence problems, or an unreliable comparison. The TRADES dynamical fit in Section 6 returns e≈0.08 for all three planets (with a half-Gaussian prior, sigma=0.083), which is in tension with a strongly circular solution. Because the RV semi-amplitudes are small, a bias of even a few tenths of m/s from unmodeled eccentricity could shift Mb and Md by more than their formal errors. Please provide a more robust test than the reported ΔBIC, for example a fixed-eccentricity grid for e in [0, 0.15], an injection-recovery study at K_b and K_d with e≈0.08, or a rerun of the eccentric fit with a better-converging sampler/parameterization, and show quantitatively how K_b and K_d, hence Mb and Md, depend on the eccentricity assumption.
  2. [Section 5.3 and Tables 3-4] The injection-recovery tests are used to argue that stellar activity explains the RV non-detection of planet c and to quantify signal suppression at P_rot. However, they do not test the recovery of the small semi-amplitudes of b and d under the adopted activity model and breakpoint detrending. Since K_b and K_d are only 3.8σ and 4.5σ detections and are of the same order as the RV jitter, an injection test at Pb and Pd (with and without the breakpoint model) would show whether the fitted K values are biased by the de-trending procedure. In addition, the injection tests assume circular orbits; given major comment 1, repeating them for e≈0.08 would directly quantify the potential mass bias. Without such tests, the quoted mass uncertainties (Table 2) likely understate the true systematic error budget.
minor comments (4)
  1. [Section 5.1 vs Table 2] The text in Section 5.1 gives 3σ upper limits K_c^up = 1.2 m/s, M_c^up = 4.0 Mearth, and rho_c^up = 3.1 g/cm3, while Table 2 note (c) gives M_c^up = 3.8 Mearth and rho_c^up = 2.9 g/cm3; please harmonize these values.
  2. [Section 4] The sentence "imposing uniform priors on (sqrt(e) cos(omega), sqrt(e) cos(omega))" contains a typo; the second coordinate should be sqrt(e) sin(omega).
  3. [Section 5.3] The statement that the recovery of injected signals at P_c implies that "the destructive interference between the RV signals induced by the star and by planet c has already occurred" is not the only possible interpretation; the original K_c may simply be small because planet c is low-mass. Please clarify the logic or soften the wording, especially since the upper limit Mup,c=3.8 Mearth allows a low-mass c.
  4. [Section 6 and Figure 9] The TTV forecast with semi-amplitudes up to ~5 hours (and drifts up to ~10 hours) is derived from the MAP parameters fitted to the same TTV data; the paper correctly presents this as a model forecast, but the abstract and conclusions could more explicitly state that the amplitude prediction is conditional on the dynamical model and the poorly sampled TTV phase, not an observationally measured amplitude.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the planet radii and RV masses are fitted directly to independent TESS and HARPS data, and the only self-referential element is the TTV forward simulation, which is transparently a model projection rather than an independent prediction.

full rationale

The central results are derived by direct MCMC fits of the HARPS RVs and TESS photometry against Keplerian and transit models (Sects. 4 and 5), with stellar parameters anchored to Gaia parallax, PARSEC isochrones, and independent spectroscopic grids; none of these inputs encodes the output masses or densities. The e=0 assumption is justified by BIC and prior simulations, a robustness assumption rather than circularity, although the paper itself concedes that the eccentric runs showed poorer convergence (Sect. 4). The TTV forecast in Fig. 9 is a forward integration of the same MAP/posterior parameters used to fit the observed TTVs, so the 5-hour semi-amplitude projection is a model forecast rather than an independent empirical prediction; the paper explicitly labels it as "numerical simulation suggests" and does not use it as evidence for the headline masses. Self-citations (MCMCI, TRADES, isochrone placement, plaNETic) are software and method references to externally calibrated codes, and no load-bearing claim is justified solely by an author's previous result. Overall, no significant circularity.

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

The central measurements depend on a set of fitted or modeling choices, chiefly the circular orbit assumption, the breakpoint activity de-trending, and the BIC-selected polynomial baselines. None of these are new physical entities; they are standard data-analysis choices. No invented particles or forces.

free parameters (5)
  • RV jitter (sigma_HARPS) = 1.49 m/s (posterior median)
    Added in quadrature to RV uncertainties in the joint MCMC fit to account for stellar activity and instrument noise; affects mass uncertainties and the significance of the K detections.
  • Breakpoint location in RV time series = Observation 48 (BJD 2458667.94)
    Chosen by BIC to split the RV series into two segments; the segmentation defines which activity polynomial is subtracted and thus affects the derived masses.
  • Planet eccentricities = 0 (fixed)
    Set to zero for all planets in the joint LC/RV fit; the alternative eccentric solution is disfavored by BIC but the assumption can bias masses if wrong.
  • Stellar rotation period P_rot = 6.7 ± 1.3 d
    Inferred from log R'HK relations and periodograms; used as the reference period for the injection tests that explain the non-detection of planet c. It is an input rather than a fitted parameter of the planetary fit.
  • Polynomial detrending orders = Per-light-curve and per-segment orders (Table A.2)
    Selected by BIC for each TESS light curve and RV segment; the de-trending baseline affects transit depths and RV signals.
assumptions (5)
  • domain assumption Planets move on Keplerian orbits with e=0 in the joint LC/RV fit.
    Invoked in Section 4: 'we set the eccentricity e = 0... for all planets.' The masses depend on this circular-orbit model.
  • domain assumption Stellar activity RV signal can be removed by segment-wise polynomial de-trending with one breakpoint.
    Invoked in Section 3.2 and Section 5.3; the breakpoint method assumes piecewise-stationary activity correlations.
  • domain assumption The anti-correlated TTV pattern between b and c is due to mutual gravitational interaction, confirming membership of c.
    Section 5.2 and Fig. A.1; alternative explanations (e.g., systematics) are not quantitatively modeled.
  • domain assumption Stellar parameters from isochrone placement (Mstar, Rstar) are correct within quoted uncertainties.
    Section 2; planet masses and radii scale with stellar mass and radius.
  • domain assumption The stellar rotation period is ~6.7 d, close to Pc, so that activity hides planet c's RV signal.
    Section 5.3; supported by periodograms and gyrochronology, but the exact period is uncertain (6-8 d range, aliases).

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Cite this review

Pith. "Pith review of Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396." pith.science (2026). https://pith.science/paper/MK7TUQSE

@misc{pith2026241114911,
  author       = {Pith},
  title        = {Pith review of: Radii, masses, and transit-timing variations of the three-planet system orbiting the naked-eye star TOI-396},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MK7TUQSE}},
  note         = {Machine review of arXiv:2411.14911}
}
abstract

TOI-396 is an F6V star ($V\approx6.4$) orbited by three transiting planets. The orbital periods of the two innermost planets are close to the 5:3 commensurability ($P_b \sim3.6$ d and $P_c \sim6.0$ d). To measure the masses of the three planets, refine their radii, and investigate whether planets b and c are in MMR, we carried out HARPS RV observations and retrieved photometric data from TESS. We extracted the RVs via a skew-normal fit onto the HARPS CCFs and performed an MCMC joint analysis of the Doppler measurements and transit photometry, while employing the breakpoint method to remove stellar activity from the RV time series. We also performed a thorough TTV dynamical analysis of the system. Our analysis confirms that the three planets have similar sizes: $R_b=2.004_{-0.047}^{+0.045}R_{\oplus}$; $R_c=1.979_{-0.051}^{+0.054}R_{\oplus}$; $R_d=2.001_{-0.064}^{+0.063}R_{\oplus}$. For the first time, we have determined the RV masses for TOI-396b and d: $M_b=3.55_{-0.96}^{+0.94}M_{\oplus}$ ($\rho_b=2.44_{-0.68}^{+0.69}$ g cm$^{-3}$) and $M_d=7.1\pm1.6M_{\oplus}$ ($\rho_d=4.9_{-1.1}^{+1.2}$ g cm$^{-3}$). Our results suggest a quite unusual system architecture, with the outermost planet being the densest. The Doppler reflex motion induced by TOI-396c remains undetected in our RV time series, likely due to the proximity of $P_c$ to the star's rotation period ($P_{\mathrm{rot}}=6.7\pm1.3$ d). We also discovered that TOI-396b and c display significant TTVs. While the TTV dynamical analysis returns a formally precise mass for TOI-396c ($M_{c,\mathrm{dyn}}=2.24^{+0.13}_{-0.67}M_{\oplus}$), the result might not be accurate owing to the poor sampling of the TTV phase. We also conclude that TOI-396b and c are close to but out of the 5:3 MMR. Our numerical simulation suggests TTV semi-amplitudes of up to 5 hours over a temporal baseline of $\sim$5.2 years.

Figures

Figures reproduced from arXiv: 2411.14911 by the authors.

Figure 1
Figure 1. TESS detrended and phase-folded LCs (blue dots) of TOI￾396 b (Top panel), TOI-396 c (Middle panel), and TOI-396 d (Bottom panel) with the transit model superimposed in red. The black markers are the binned data points (binning 20 min). 2011a; Haywood et al. 2014; Suárez Mascareño et al. 2017; Gan￾dolfi et al. 2017). A possible explanation for the non-detection of the Doppler reflex motion induced by TOI-396 c is tha… view at source ↗
Figure 3
Figure 3. Mass-radius diagram showing the three planets orbiting [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 2
Figure 2. HARPS detrended and phase-folded RV time series of TOI-396 b (Top panel), TOI-396 c (Middle panel), and TOI￾396 d (Bottom panel) with the Keplerian model superimposed in red. For each planet, the time series were obtained after sub￾tracting the RV contribution of the other planets. The error bars also account for the jitter contribution (displayed in grey). described above and remove this signal by fitting a quadrat… view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: TTV amplitudes obtained for TOI-396 b (Top panel), TOI-396 c (Middle panel), and TOI-396 d (Bottom panel). The grey shaded region highlights the 1σ uncertainty region as de￾rived from error propagation of the linear ephemerides. as the 6–8 d rotation period signals we …
Figure 5
Figure 5. Figure 5: Time series (left panels) and GLS periodograms (right panels) of the line profile variation diagnostics and activity indicators [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
Figure 6
Figure 6. Figure 6: Observed minus calculated synthetic diagrams derived from the joint RV and TTV dynamical analysis with TRADES for [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]
Figure 7
Figure 7. Figure 7: Left panel: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_7.png]
Figure 8
Figure 8. Figure 8: Temporal evolution of the critical resonance angles [PITH_FULL_IMAGE:figures/full_fig_p013_8.png]
Figure 9
Figure 9. Figure 9: Synthetic O − C diagrams obtained after performing for￾ward numerical N-body simulations with TRADES (integration of 5.2 years). The C represents the timings calculated from the linear ephemerides in [PITH_FULL_IMAGE:figures/full_fig_p014_9.png]
Figure 10
Figure 10. Figure 10: Inferred posteriors for the most important internal structure parameters of TOI-396 b. The depicted parameters are the mass [PITH_FULL_IMAGE:figures/full_fig_p015_10.png]
Figure 11
Figure 11. Figure 11: Same as Figure 10 but for TOI-396 d [PITH_FULL_IMAGE:figures/full_fig_p015_11.png]
Figure 12
Figure 12. Figure 12: Transit (top panel) and eclipse (bottom panel) spectro￾scopic metrics for the TOI-396 planets (see legend). The metrics were calculated using the 2MASS Ks-band magnitude. The grey markers show the metrics for the known sample of transiting ex￾oplanets to date. The blu…

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Works this paper leans on

146 extracted references · 40 canonical work pages · cited by 1 Pith paper

  1. [1]

    J., Wittenmyer, R

    Addison, B., Wright, D. J., Wittenmyer, R. A., et al. 2019, PASP, 131, 115003

    2019

  2. [2]

    G., et al

    Adibekyan, V ., Dorn, C., Sousa, S. G., et al. 2021, Science, 374, 330

    2021

  3. [3]

    C., et al

    Adibekyan, V ., Figueira, P., Santos, N. C., et al. 2015, A&A, 583, A94

    2015

  4. [4]

    Z., Sousa, S

    Adibekyan, V . Z., Sousa, S. G., Santos, N. C., et al. 2012, A&A, 545, A32

    2012

  5. [5]

    & Fabrycky, D

    Agol, E. & Fabrycky, D. C. 2018, in Handbook of Exoplanets, ed. H. J. Deeg & J. A. Belmonte (Cambridge University Press), 7

    2018

  6. [6]

    2005, MNRAS, 359, 567

    Agol, E., Steffen, J., Sari, R., & Clarkson, W. 2005, MNRAS, 359, 567

    2005

  7. [7]

    2021, ApJ, 914, 84

    Aguichine, A., Mousis, O., Deleuil, M., & Marcq, E. 2021, ApJ, 914, 84

    2021

  8. [8]

    Alexander, R. D. & Armitage, P. J. 2009, ApJ, 704, 989 Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33

    2009

Show all 146 references
  1. [9]

    & Perron, P

    Bai, J. & Perron, P. 2003, Journal of Applied Econometrics, 18, 1

    2003

  2. [10]

    1996, A&AS, 119, 373

    Baranne, A., Queloz, D., Mayor, M., et al. 1996, A&AS, 119, 373

    1996

  3. [11]

    Barnes, S. A. 2010, ApJ, 722, 222

    2010

  4. [12]

    2021, Experimental Astronomy, 51, 109

    Benz, W., Broeg, C., Fortier, A., et al. 2021, Experimental Astronomy, 51, 109

    2021

  5. [13]

    B., Öberg, K

    Bergner, J. B., Öberg, K. I., Bergin, E. A., et al. 2020, ApJ, 898, 97

    2020

  6. [14]

    J., et al

    Bonfanti, A., Delrez, L., Hooton, M. J., et al. 2021, A&A, 646, A157

    2021

  7. [15]

    A., et al

    Bonfanti, A., Gandolfi, D., Egger, J. A., et al. 2023, A&A, 671, L8

    2023

  8. [16]

    & Gillon, M

    Bonfanti, A. & Gillon, M. 2020, A&A, 635, A6

    2020

  9. [17]

    2016, A&A, 585, A5

    Bonfanti, A., Ortolani, S., & Nascimbeni, V . 2016, A&A, 585, A5

    2016

  10. [18]

    2015, A&A, 575, A18

    Bonfanti, A., Ortolani, S., Piotto, G., & Nascimbeni, V . 2015, A&A, 575, A18

    2015

  11. [19]

    2024, A&A, 689, A52

    Borsato, L., Degen, D., Leleu, A., et al. 2024, A&A, 689, A52

    2024

  12. [20]

    2019, MNRAS, 484, 3233

    Borsato, L., Malavolta, L., Piotto, G., et al. 2019, MNRAS, 484, 3233

    2019

  13. [21]

    2014, A&A, 571, A38

    Borsato, L., Marzari, F., Nascimbeni, V ., et al. 2014, A&A, 571, A38

    2014

  14. [22]

    2021, MNRAS, 506, 3810

    Borsato, L., Piotto, G., Gandolfi, D., et al. 2021, MNRAS, 506, 3810

    2021

  15. [23]

    2002, A&A, 390, 779

    Borysow, A. 2002, A&A, 390, 779

    2002

  16. [24]

    G., & Fu, Y

    Borysow, A., Jorgensen, U. G., & Fu, Y . 2001, J. Quant. Spectr. Rad. Transf., 68, 235

    2001

  17. [25]

    E., Phillip, C., Fleming, S

    Brasseur, C. E., Phillip, C., Fleming, S. W., Mullally, S. E., & White, R. L. 2019, Astrocut: Tools for creating cutouts of TESS images, Astrophysics Source Code Library, record ascl:1905.007

    2019

  18. [26]

    2010, A&A, 519, A51

    Bruntt, H., Deleuil, M., Fridlund, M., et al. 2010, A&A, 519, A51

    2010

  19. [27]

    S., & Sharp, C

    Burrows, A., Marley, M. S., & Sharp, C. M. 2000, ApJ, 531, 438

    2000

  20. [28]

    R., Fabrycky, D

    Ciardi, D. R., Fabrycky, D. C., Ford, E. B., et al. 2013, ApJ, 763, 41

    2013

  21. [29]

    Correia, A. C. M., Delisle, J.-B., & Laskar, J. 2018, in Handbook of Exoplanets, ed. H. J. Deeg & J. A. Belmonte (Springer International Publishing AG, part of Springer Nature), 12

    2018

  22. [30]

    Cubillos, P. E. 2017, ApJ, 850, 32

    2017

  23. [31]

    Cubillos, P. E. & Blecic, J. 2021, MNRAS, 505, 2675

    2021

  24. [32]

    M., Skrutskie, M

    Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, 2MASS All Sky Catalog of point sources. (University of Massachusetts and Infrared Processing and Analysis Center (IPAC/California Institute of Technology)) D’Angelo, G. & Lubow, S. H. 2008, ApJ, 685, 560

    2003

  25. [33]

    B., Laskar, J., Correia, A

    Delisle, J. B., Laskar, J., Correia, A. C. M., & Boué, G. 2012, A&A, 546, A71

    2012

  26. [34]

    2021, Nature Astronomy, 5, 775

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

    2021

  27. [35]

    2017, A&A, 597, A37

    Dorn, C., Venturini, J., Khan, A., et al. 2017, A&A, 597, A37

    2017

  28. [36]

    P., Davies, G

    Doyle, A. P., Davies, G. R., Smalley, B., Chaplin, W. J., & Elsworth, Y . 2014, MNRAS, 444, 3592

    2014

  29. [37]

    R., Henry, G

    Dragomir, D., Kane, S. R., Henry, G. W., et al. 2012, ApJ, 754, 37

    2012

  30. [38]

    A., Osborn, H

    Egger, J. A., Osborn, H. P., Kubyshkina, D., et al. 2024, A&A, 688, A223

    2024

  31. [39]

    & Jordán, A

    Espinoza, N. & Jordán, A. 2015, MNRAS, 450, 1879

    2015

  32. [40]

    C., Lissauer, J

    Fabrycky, D. C., Lissauer, J. J., Ragozzine, D., et al. 2014, ApJ, 790, 146

    2014

  33. [41]

    2019, The Journal of Open Source Software, 4, 1864

    Foreman-Mackey, D., Farr, W., Sinha, M., et al. 2019, The Journal of Open Source Software, 4, 1864

    2019

  34. [42]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306

    2013

  35. [43]

    Y ., Bonfanti, A., et al

    Fridlund, M., Georgieva, I. Y ., Bonfanti, A., et al. 2024, A&A, 684, A12 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1

    2024

  36. [44]

    P., et al

    Gandolfi, D., Barragán, O., Hatzes, A. P., et al. 2017, AJ, 154, 123

    2017

  37. [45]

    P., Mather, J

    Gardner, J. P., Mather, J. C., Clampin, M., et al. 2006, Space Sci. Rev., 123, 485

    2006

  38. [46]

    & Rubin, D

    Gelman, A. & Rubin, D. B. 1992, Statistical Science, 7, 457

    1992

  39. [47]

    Geweke, J. F. 1991, Evaluating the accuracy of sampling-based approaches to the calculation of posterior moments, Staff Report 148, Federal Reserve Bank of Minneapolis

    1991

  40. [48]

    M., Brasseur, C

    Ginsburg, A., Sip˝ocz, B. M., Brasseur, C. E., et al. 2019, AJ, 157, 98

    2019

  41. [49]

    & Tremaine, S

    Goldreich, P. & Tremaine, S. 1980, ApJ, 241, 425

    1980

  42. [50]

    & Weare, J

    Goodman, J. & Weare, J. 2010, Communications in Applied Mathematics and Computational Science, 5, 65

    2010

  43. [51]

    O., Corbally, C

    Gray, R. O., Corbally, C. J., Garrison, R. F., et al. 2006, AJ, 132, 161

    2006

  44. [52]

    2024, A&A, 681, A96

    Haldemann, J., Dorn, C., Venturini, J., Alibert, Y ., & Benz, W. 2024, A&A, 681, A96

    2024

  45. [53]

    N., White, T

    Handberg, R., Lund, M. N., White, T. R., et al. 2021, AJ, 162, 170

    2021

  46. [54]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357

    2020

  47. [55]

    Hatzes, A. P. 2016, in Astrophysics and Space Science Library, V ol. 428, Meth- ods of Detecting Exoplanets: 1st Advanced School on Exoplanetary Science, ed. V . Bozza, L. Mancini, & A. Sozzetti, 3

    2016

  48. [56]

    Hatzes, A. P. 2019, The Doppler Method for the Detection of Exoplanets (Insti- tute of Physics Publishing)

    2019

  49. [57]

    P., Dvorak, R., Wuchterl, G., et al

    Hatzes, A. P., Dvorak, R., Wuchterl, G., et al. 2010, A&A, 520, A93

    2010

  50. [58]

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

    Haywood, R. D., Collier Cameron, A., Queloz, D., et al. 2014, MNRAS, 443, 2517 Høg, E., Fabricius, C., Makarov, V . V ., et al. 2000, A&A, 355, L27

    2014

  51. [59]

    J., Fabrycky, D

    Holman, M. J., Fabrycky, D. C., Ragozzine, D., et al. 2010, Science, 330, 51

    2010

  52. [60]

    J., Winn, J

    Holman, M. J., Winn, J. N., Latham, D. W., et al. 2006, ApJ, 652, 1715

    2006

  53. [61]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90

    2007

  54. [62]

    N., et al

    Izidoro, A., Ogihara, M., Raymond, S. N., et al. 2017, MNRAS, 470, 1750

    2017

  55. [63]

    M., Twicken, J

    Jenkins, J. M., Twicken, J. D., McCauli ff, S., et al. 2016, in Society of Photo- Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 9913, Soft- ware and Cyberinfrastructure for Astronomy IV , ed. G. Chiozzi & J. C. Guz- man, 99133E

    2016

  56. [64]

    Kass, R. E. & Raftery, A. E. 1995, Journal of the American Statistical Associa- tion, 90, 773

    1995

  57. [65]

    Kempton, E. M. R., Bean, J. L., Louie, D. R., et al. 2018, PASP, 130, 114401

    2018

  58. [66]

    Kipping, D. M. 2010, MNRAS, 408, 1758

    2010

  59. [67]

    2022, A&A, 666, A143

    Kossakowski, D., Kürster, M., Henning, T., et al. 2022, A&A, 666, A143

    2022

  60. [68]

    Kuerster, M., Schmitt, J. H. M. M., Cutispoto, G., & Dennerl, K. 1997, A&A, 320, 831

    1997

  61. [69]

    Kurucz, R. L. 1970, SAO Special Report, 309

    1970

  62. [70]

    Kurucz, R. L. 1993, SYNTHE spectrum synthesis programs and line data (As- trophysics Source Code Library)

    1993

  63. [71]

    Kurucz, R. L. 2013, ATLAS12: Opacity sampling model atmosphere program

    2013

  64. [72]

    1997, A&A, 317, L75

    Laskar, J. 1997, A&A, 317, L75

    1997

  65. [73]

    2000, Phys

    Laskar, J. 2000, Phys. Rev. Lett., 84, 3240

    2000

  66. [74]

    & Petit, A

    Laskar, J. & Petit, A. C. 2017, A&A, 605, A72

    2017

  67. [75]

    Lee, M. H. & Peale, S. J. 2002, arXiv e-prints, astro

    2002

  68. [76]

    C., et al

    Leleu, A., Alibert, Y ., Hara, N. C., et al. 2021, A&A, 649, A26

    2021

  69. [77]

    I., Zhu, Z., & Ste ffen, J

    Li, M., Huang, S., Petaev, M. I., Zhu, Z., & Ste ffen, J. H. 2020, MNRAS, 495, 2543 Lightkurve Collaboration, Cardoso, J. V . d. M., Hedges, C., et al. 2018, Lightkurve: Kepler and TESS time series analysis in Python, Astrophysics Source Code Library

    2020

  70. [78]

    Lin, D. N. C. & Papaloizou, J. 1979, MNRAS, 186, 799

    1979

  71. [79]

    2021, A&A, 649, A4

    Lindegren, L., Bastian, U., Biermann, M., et al. 2021, A&A, 649, A4

    2021

  72. [80]

    J., Ragozzine, D., Fabrycky, D

    Lissauer, J. J., Ragozzine, D., Fabrycky, D. C., et al. 2011, ApJS, 197, 8

    2011

  73. [81]

    & Pepe, F

    Lovis, C. & Pepe, F. 2007, A&A, 468, 1115

    2007

  74. [82]

    N., Handberg, R., Buzasi, D

    Lund, M. N., Handberg, R., Buzasi, D. L., et al. 2021, ApJS, 257, 53

    2021

  75. [83]

    P., Leleu, A., et al

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

    2023

  76. [84]

    Mamajek, E. E. & Hillenbrand, L. A. 2008, ApJ, 687, 1264

    2008

  77. [85]

    2017, ApJ, 835, 77

    Marigo, P., Girardi, L., Bressan, A., et al. 2017, ApJ, 835, 77

    2017

  78. [86]

    2003, The Messenger, 114, 20

    Mayor, M., Pepe, F., Queloz, D., et al. 2003, The Messenger, 114, 20

    2003

  79. [87]

    J., DiSanti, M

    McKay, A. J., DiSanti, M. A., Kelley, M. S. P., et al. 2019, AJ, 158, 128

    2019

  80. [88]

    2023, A&A, 670, A68

    Mishra, L., Alibert, Y ., Udry, S., & Mordasini, C. 2023, A&A, 670, A68

    2023

  81. [89]

    Morton, T. D. 2012, ApJ, 761, 6

    2012

  82. [90]

    Morton, T. D. 2015, VESPA: False positive probabilities calculator, Astrophysics Source Code Library, record ascl:1503.011

    2015

  83. [91]

    Mumma, M. J. & Charnley, S. B. 2011, ARA&A, 49, 471

    2011

  84. [92]

    A., Hearnshaw, J

    Murdoch, K. A., Hearnshaw, J. B., & Clark, M. 1993, ApJ, 413, 349

    1993

  85. [93]

    2024, A&A, 690, A349

    Nascimbeni, V ., Borsato, L., Leonardi, P., et al. 2024, A&A, 690, A349

    2024

  86. [94]

    2023, A&A, 673, A42

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

    2023

  87. [95]

    B., & Payne, M

    Nelson, B., Ford, E. B., & Payne, M. J. 2014, ApJS, 210, 11

    2014

  88. [96]

    W., Hartmann, L

    Noyes, R. W., Hartmann, L. W., Baliunas, S. L., Duncan, D. K., & Vaughan, A. H. 1984, ApJ, 279, 763

    1984

  89. [97]

    F., Helled, R., & Bouchy, F

    Otegi, J. F., Helled, R., & Bouchy, F. 2022, A&A, 658, A107

    2022

  90. [98]

    2016, A&A, 585, A114

    Parviainen, H., Pallé, E., Nortmann, L., et al. 2016, A&A, 585, A114

    2016

  91. [99]

    2002, A&A, 388, 632

    Pepe, F., Mayor, M., Galland, F., et al. 2002, A&A, 388, 632

    2002

  92. [100]

    Perryman, M. A. C., Lindegren, L., Kovalevsky, J., et al. 1997, A&A, 323, L49

    1997

  93. [101]

    M., Fridlund, M., Barragán, O., et al

    Persson, C. M., Fridlund, M., Barragán, O., et al. 2018, A&A, 618, A33

    2018

  94. [102]

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

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

    2018

  95. [103]

    A., Howard, A

    Petigura, E. A., Howard, A. W., Lopez, E. D., et al. 2016, ApJ, 818, 36

    2016

  96. [104]

    C., Laskar, J., & Boué, G

    Petit, A. C., Laskar, J., & Boué, G. 2018, A&A, 617, A93

    2018

  97. [105]

    & Valenti, J

    Piskunov, N. & Valenti, J. A. 2017, A&A, 597, A16

    2017

  98. [106]

    E., Kupka, F., Ryabchikova, T

    Piskunov, N. E., Kupka, F., Ryabchikova, T. A., Weiss, W. W., & Jeffery, C. S. 1995, A&AS, 112, 525

    1995

  99. [107]

    2006, MNRAS, 373, 231 Article number, page 17 of 25 A&A proofs: manuscript no

    Pont, F., Zucker, S., & Queloz, D. 2006, MNRAS, 373, 231 Article number, page 17 of 25 A&A proofs: manuscript no. TOI-396

    2006

  100. [108]

    M., Pickering, T

    Pontoppidan, K. M., Pickering, T. E., Laidler, V . G., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 9910, Observatory Operations: Strategies, Processes, and Systems VI, ed. A. B. Peck, R. L. Seaman, & C. R. Benn, 991016

    2016

  101. [109]

    W., Sivan, J

    Queloz, D., Henry, G. W., Sivan, J. P., et al. 2001, A&A, 379, 279

    2001

  102. [110]

    & Liu, S

    Rein, H. & Liu, S. F. 2012, A&A, 537, A128

    2012

  103. [111]

    & Tamayo, D

    Rein, H. & Tamayo, D. 2015, MNRAS, 452, 376

    2015

  104. [112]

    E., Rothman, L

    Richard, C., Gordon, I. E., Rothman, L. S., et al. 2012, J. Quant. Spectr. Rad. Transf., 113, 1276

    2012

  105. [113]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical

    2015

  106. [114]

    S., Gordon, I

    Rothman, L. S., Gordon, I. E., Barber, R. J., et al. 2010, J. Quant. Spectr. Rad. Transf., 111, 2139

    2010

  107. [115]

    C., Sousa, S

    Santos, N. C., Sousa, S. G., Mortier, A., et al. 2013, A&A, 556, A150

    2013

  108. [116]

    1978, Annals of Statistics, 6, 461

    Schwarz, G. 1978, Annals of Statistics, 6, 461

    1978

  109. [117]

    2022, A&A, 664, A127

    Simola, U., Bonfanti, A., Dumusque, X., et al. 2022, A&A, 664, A127

    2022

  110. [118]

    2019, A&A, 622, A131

    Simola, U., Dumusque, X., & Cisewski-Kehe, J. 2019, A&A, 622, A131

    2019

  111. [119]

    C., Stumpe, M

    Smith, J. C., Stumpe, M. C., Van Cleve, J. E., et al. 2012, PASP, 124, 1000

    2012

  112. [120]

    Sneden, C. A. 1973, PhD thesis, THE UNIVERSITY OF TEXAS AT AUSTIN

    1973

  113. [121]

    Sousa, S. G. 2014, in Determination of Atmospheric Parameters of B-, A-, F- and G-Type Stars., ed. E. Niemczura, B. Smalley, & W. Pych (Springer Inter- national Publishing (Cham)), 297–310

    2014

  114. [122]

    G., Adibekyan, V ., Delgado-Mena, E., et al

    Sousa, S. G., Adibekyan, V ., Delgado-Mena, E., et al. 2021, A&A, 656, A53

    2021

  115. [123]

    G., Santos, N

    Sousa, S. G., Santos, N. C., Adibekyan, V ., Delgado-Mena, E., & Israelian, G. 2015, A&A, 577, A67

    2015

  116. [124]

    G., Santos, N

    Sousa, S. G., Santos, N. C., Israelian, G., Mayor, M., & Monteiro, M. J. P. F. G. 2007, A&A, 469, 783

    2007

  117. [125]

    G., Santos, N

    Sousa, S. G., Santos, N. C., Mayor, M., et al. 2008, A&A, 487, 373

    2008

  118. [126]

    & Price, K

    Storn, R. & Price, K. 1997, Journal of Global Optimization, 11, 341

    1997

  119. [127]

    C., Smith, J

    Stumpe, M. C., Smith, J. C., Catanzarite, J. H., et al. 2014, PASP, 126, 100

    2014

  120. [128]

    C., Smith, J

    Stumpe, M. C., Smith, J. C., Van Cleve, J. E., et al. 2012, PASP, 124, 985 Suárez Mascareño, A., Rebolo, R., González Hernández, J. I., & Esposito, M. 2017, MNRAS, 468, 4772

    2012

  121. [129]

    Sundman, K. F. 1913, Acta Mathematica, 36, 105

    1913

  122. [130]

    Tanaka, H., Takeuchi, T., & Ward, W. R. 2002, ApJ, 565, 1257

    2002

  123. [131]

    N., Al-Refaie, A

    Tennyson, J., Yurchenko, S. N., Al-Refaie, A. F., et al. 2016, Journal of Molecu- lar Spectroscopy, 327, 73 ter Braak, C. J. F. & Vrugt, J. A. 2008, Statistics and Computing, 18, 435

    2016

  124. [132]

    2014, A&A, 562, A27

    Thiabaud, A., Marboeuf, U., Alibert, Y ., et al. 2014, A&A, 562, A27

    2014

  125. [133]

    2015, A&A, 574, A138

    Thiabaud, A., Marboeuf, U., Alibert, Y ., Leya, I., & Mezger, K. 2015, A&A, 574, A138

    2015

  126. [134]

    2007, MNRAS, 378, 72 Van Eylen, V ., Albrecht, S., Huang, X., et al

    Trotta, R. 2007, MNRAS, 378, 72 Van Eylen, V ., Albrecht, S., Huang, X., et al. 2019, AJ, 157, 61

    2007

  127. [135]

    X., Rodriguez, J

    Vanderburg, A., Huang, C. X., Rodriguez, J. E., et al. 2019, ApJ, 881, L19

    2019

  128. [136]

    A., et al

    Vanderburg, A., Plavchan, P., Johnson, J. A., et al. 2016, MNRAS, 459, 3565

    2016

  129. [137]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261

    2020

  130. [138]

    2015, A&A, 582, A88

    Walsh, C., Nomura, H., & van Dishoeck, E. 2015, A&A, 582, A88

    2015

  131. [139]

    Weiss, L. M. & Marcy, G. W. 2014, ApJ, 783, L6

    2014

  132. [140]

    M., Marcy, G

    Weiss, L. M., Marcy, G. W., Petigura, E. A., et al. 2018, AJ, 155, 48

    2018

  133. [141]

    2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol

    Wildi, F., Pepe, F., Chazelas, B., Lo Curto, G., & Lovis, C. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S

    2010

  134. [142]

    Winn, J. N. 2010, in Exoplanets, ed. S. Seager (University of Arizona Press,

    2010

  135. [143]

    Winn, J. N. & Fabrycky, D. C. 2015, ARA&A, 53, 409

    2015

  136. [144]

    & Holman, M

    Wisdom, J. & Holman, M. 1991, AJ, 102, 1528

    1991

  137. [145]

    & Kürster, M

    Zechmeister, M. & Kürster, M. 2009, A&A, 496, 577 1 Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria e-mail: andrea.bonfanti@oeaw.ac.at 2 Dipartimento di Fisica, Università degli Studi di Torino, via Pietro Giuria 1, I-10125, Torino, Italy 3 Department of ...

    2009

  138. [146]

    Studies, SOKENDAI, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan 31 Instituto de Astrofísica de Canarias (IAC), calle Vía Láctea s /n, 38205 La Laguna, Tenerife, Spain 32 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206 La Laguna, Tenerife, Spain 33 Institute...

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