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A four-planet system orbiting the old thick disk star TOI-1203

T0 review · 2 major / 4 minor · reviewed 2026-08-04 · deepseek-v4-flash

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Pith's one-line read Four planets orbit a 12.5-billion-year-old thick-disk star, the paper shows.

desk verdict Solid characterization paper: three new planets around an old thick-disk star, two with precisely measured masses and radii; the two RV-only planets are the main residual risk, but the evidence is strong. read the letter →

arxiv 2509.10136 v1 pith:UFXVYMXB submitted 2025-09-12 astro-ph.EP astro-ph.SR

D. Gandolfi , A. Alnajjarine , L. M. Serrano , J. A. Egger , K. W. F. Lam , J. Cabrera , A. P. Hatzes , M. Fridlund
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M. Garbaccio Gili T. G. Wilson W. D. Cochran A. Brandeker E. Goffo S. G. Sousa G. Nowak A. Heitzmann C. Hellier J. Venturini J. Livingston A. Bonfanti O. Barragán V. Adibekyan E. Knudstrup Y. Alibert S. Grziwa C. Ziegler L. Fossati F. Murgas A. C. M. Correia S. H. Albrecht J. Laskar E. W. Guenther S. J.A.J. Salmon S. Redfield N. Billot H. J. Deeg L. Delrez L. Palethorpe V. Van Eylen F. Rodler J. Alarcon J. M. Jenkins J. D. Twicken A. W. Mann R. Alonso J. Asquier T. Bárczy D. Barrado S. C. C. Barros W. Baumjohann W. Benz L. Borsato C. Broeg M. Buder P. Chaturvedi A. Collier Cameron Sz. Csizmadia P. E. Cubillos M. B. Davies M. Deleuil A. Deline O. D. S. Demangeon B.-O. Demory A. Derekas B. Edwards D. Ehrenreich A. Erikson A. Fortier K. Gazeas M. Gillon M. Güdel M. N. Günther Ch. Helling K. G. Isaak L. L. Kiss J. Korth N. Law A. Lecavelier des Etangs A. Leleu M. Lendl P. Leonardi D. Magrin G. Mantovan L. Marafatto P. F. L. Maxted M. Mecina B. Merín C. Mordasini V. Nascimbeni A. Nigioni G. Olofsson H. P. Osborn R. Ottensamer I. Pagano E. Pallé C. M. Persson G. Peter D. Piazza G. Piotto D. Pollacco D. Queloz R. Ragazzoni N. Rando H. Rauer I. Ribas G. R. Ricker N. C. Santos G. Scandariato S. Seager D. Ségransan A. E. Simon A. M. S. Smith M. Stalport S. Sulis Gy. M. Szabó S. Udry S. Ulmer-Moll V. Van Grootel E. Villaver N. A. Walton J. N. Winn S. Wolf T. Zingales
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords four-planetsystemsuper-Earthsub-Neptuneradialvelocitytransitphotometrythickdiskstellarabundancesdynamicalstability
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

The paper reports that the bright G3V star TOI-1203, a 12.5-billion-year-old, alpha-element-enhanced member of the galactic thick disk, hosts four planets: a transiting super-Earth on a 4.2-day orbit, a non-transiting super-Earth on a 13.1-day orbit, the previously known transiting sub-Neptune on a 25.5-day orbit (now with a measured mass), and a non-transiting eccentric Neptune-mass planet on a 204.6-day orbit. Masses and radii of the two transiting planets are measured to 8-9% precision, and dynamical integrations find configurations stable over billion-year timescales. If correct, this is one of the oldest known multi-planet systems, with implications for when rocky planets could form in the metal-poor early galaxy. The paper also identifies a ~615-day variation in the HARPS instrumental profile that leaves no detectable imprint on the radial velocities, a cautionary result for ultra-precise Doppler surveys.

What carries the argument

The analysis rests on a joint Markov-chain Monte Carlo fit of TESS and CHEOPS transit light curves together with HARPS radial velocities modeled as four Keplerians, combined with iterative pre-whitening of GLS periodograms to isolate the Doppler signals. The long-period systematic in the HARPS line-profile FWHM is diagnosed by comparing the CCF FWHM against the FWHM of Th-Ar calibration lines, identifying a ~615-day instrumental profile variation. Dynamical stability is assessed with global frequency analysis maps and long symplectic integrations, and internal compositions are inferred from mass-radius modeling.

What would settle it

Two more years of high-precision radial velocities tracking the 204.6-day signal through at least two additional cycles: if it is not coherent as a single Keplerian, or if modeling the instrument-profile variation removes it, the planetary interpretation of TOI-1203 e collapses. A secondary check would be detecting transits of c or e, which the paper argues are unlikely but which would settle their geometry.

Watch

Extended reading notes

Core claim

TOI-1203 is a four-planet system. The 25.5-day transiting sub-Neptune previously flagged by TESS is spectroscopically confirmed, with its mass determined (7.39±0.62 M⊕) and radius refined (2.918 R⊕). A new transiting super-Earth, TOI-1203 b, is confirmed by CHEOPS photometry with mass 3.51 M⊕ and radius 1.52 R⊕. Two additional Doppler signals at 13.1 and 204.6 days are attributed to planets with minimum masses 5.46 and 42.10 M⊕; the outer planet is eccentric (e=0.152). The host is an old (12.5 Gyr), metal-poor, alpha-enhanced thick-disk star. Stability maps show the system is stable for Gyr, sits near but not inside mean-motion resonances, and has the pericenters of c and d anti-aligned. A l

Load-bearing premise

The 13.1-day and 204.6-day radial-velocity signals are genuine planets, not artifacts of the pre-whitening procedure, stellar activity, or the ~615-day instrumental profile drift whose 230-day alias sits within the frequency resolution of the 204.6-day signal.

Editorial extensions

If this is right

  • TOI-1203 b becomes one of the rare small planets whose mass and radius are both known to better than ~10%, placing it in the rocky/silicate regime of the mass-radius diagram.
  • The system straddles the radius valley, with a rocky super-Earth and a volatile-rich sub-Neptune orbiting the same old star, offering a test of how wide binaries and stellar age affect the valley's location.
  • The near-but-not-exact period commensurabilities (3:1, 2:1, 8:1) and the anti-aligned pericenters of c and d provide a benchmark for models of migration, tidal damping, and secular evolution in ancient systems.
  • The detected ~615-day instrumental profile variation, with no RV counterpart, shows that symmetric profile changes can hide in line-width diagnostics; monitoring IP shape is therefore essential for RV surveys aiming at 10 cm/s precision.

Reading between the lines

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

  • If the 204.6-day signal is confirmed as a planet, TOI-1203 will be a reference for how early-galaxy rocky planets form, since the system assembled when the universe was about 1.3 Gyr old.
  • The stability analysis maps out stable niches between b and c and between d and e; additional RV monitoring could test whether those niches are empty or occupied by smaller companions.
  • The Th-Ar line-width diagnostic used here could be reapplied to archival HARPS data to flag long-period RV signals that coincide with instrument-profile variations, potentially reclassifying some published planet candidates.
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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 reports the discovery and characterization of a four-planet system around the bright, old, metal-poor G3V star TOI-1203. Using 190 HARPS RVs, TESS and CHEOPS photometry, and a joint MCMC analysis, the authors confirm the previously known transiting sub-Neptune TOI-1203 d (P≈25.5 d, M=7.39±0.62 M⊕, R=2.918±0.045 R⊕), discover and confirm a transiting super-Earth TOI-1203 b (P≈4.16 d, M=3.51±0.33 M⊕, R=1.520±0.045 R⊕), and report two RV-only planets: TOI-1203 c (P≈13.08 d, M sin i=5.46±0.51 M⊕) and TOI-1203 e (P≈204.6 d, M sin i=42.10±1.8 M⊕, e=0.152±0.029). A stability analysis shows that configurations consistent with the data can be stable over Gyr timescales, and an interior-structure analysis of b and d is presented. The paper also identifies a ~615–630 d systematic in the HARPS CCF FWHM, traced to Th-Ar line widths, and attributes it to instrumental profile variations with no counterpart in the RVs.

Significance. If the detections hold, this is a valuable addition to the small sample of precisely characterized multi-planet systems around very old, α-enhanced thick-disk stars. The two transiting planets have masses and radii measured to better than ~10% and ~3%, respectively, placing them on the mass–radius diagram with clear compositional implications. The RV-only planets, especially the 13.1 d signal at K≈1.6 m/s, are the weakest link, and the paper would benefit from a correlated-noise robustness check. The HARPS instrumental-profile finding is an important cautionary result for precision-RV programs. Strengths include the large homogeneous HARPS dataset, the independent CHEOPS confirmation of TOI-1203 b, the use of ancillary activity indicators, the bootstrap FAP calculations, and the explicit forward stability and interior-structure checks that use the fitted parameters as inputs rather than as predictions.

major comments (2)
  1. [Sects. 4 and 9; Table B.2] The two RV-only signals (TOI-1203 c at 13.08 d with K_c=1.62±0.14 m/s, and TOI-1203 e at 204.6 d) are load-bearing for the four-planet claim. Their detection significance is established through pre-whitening with bootstrap FAPs that assume white noise, and the final fit models all noise with a single white jitter term (σ_HARPS=0.83±0.10 m/s). For a signal whose amplitude is only ~2× the jitter, unmodeled correlated noise could inflate the significance. I request a robustness check, e.g., a joint fit that includes a Gaussian-process or moving-average term for the RVs, or an injection-recovery test with red-noise residuals. This would materially increase confidence in planets c and e.
  2. [Sect. 9 and Sect. 5] The TESS Sector 36 transits of TOI-1203 b are excluded 'due to the lack of a detectable transit signal' in that sector. This is a post-hoc data selection that could bias the transit parameters and ephemeris if the non-detection is due to an unmodeled systematic rather than noise. Since CHEOPS confirms the transit near the same epoch, the exclusion likely does not affect the planet's existence, but the paper should quantify the consistency, e.g., by performing an injection-recovery test in Sector 36 or by modeling the Sector 36 data with a high-noise term.
minor comments (4)
  1. [Table B.2] The reported RV semi-amplitude for TOI-1203 d is listed as K_d=1.74±0.014 m/s. Given the values for the other planets and the mass uncertainty, the error bar is likely 0.14 m/s, not 0.014. Please check and correct.
  2. [Sect. 2] The text 'from 5 January to 2 March 2026, 2025.1' contains a stray '2025.1'; the intended date should be cleaned up.
  3. [Sect. 8.5] 'Adopting the LRS determination' should read 'LSR determination'.
  4. [Sect. 9] Typo: 'Markow chains' should be 'Markov chains'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity found: the planet parameters are fitted directly to independent RV and photometric data, and the stability and interior-structure analyses are forward consistency checks using those fitted parameters as inputs.

full rationale

The paper's central claims are the detection and characterization of four planets around TOI-1203. These are derived by directly fitting a four-Keplerian RV model to HARPS radial velocities and transit models to TESS and CHEOPS photometry (Sect. 9), with no parameter that defines the result being set by the result itself. The two RV-only planets (c and e) are identified by periodogram analysis and pre-whitening (Sect. 4), and their significance is assessed via bootstrap FAPs against the data, not against any output of the final model. The transiting planets b and d are confirmed by independent photometry (CHEOPS and TESS). The stellar parameters (Teff, [Fe/H], [alpha/Fe], age) come from separate spectroscopic, photometric, and isochrone analyses; the thick-disk classification combines these with kinematic probabilities. The stability analysis (Sect. 10) takes the fitted orbital parameters as input and checks whether any dynamically stable configuration exists; it does not generate the orbital parameters. Likewise, the interior-structure analysis (Sect. 11) uses the measured masses and radii as inputs to a forward model. The only predictive step, estimating the radius of non-transiting planet c from a mass-radius relation (Otegi et al. 2020), is an externally calibrated empirical relation used to assess transit detectability, not to define the planet's existence. Self-citations (pyaneti, DST, plaNETic, BICEPS, PIPE, pycheops) are citations to published codes/methods, not to unverified uniqueness theorems or to the present result, and none is load-bearing in a way that reduces the argument to itself. The residual scientific risk (correlated noise affecting the 13.1 d signal) is a data-quality concern, not a circularity. I therefore find no circular step and assign a score of 0.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The central claim rests on standard exoplanet detection assumptions: the RV and transit signals are planetary, and the stellar parameters are correct. No new physical entities are introduced. The main fitted parameters are the orbital elements themselves, which constitute the result rather than ad hoc inputs; the only auxiliary fitted parameters are the RV jitter and limb-darkening coefficients.

free parameters (2)
  • RV jitter sigma_HARPS = 0.83±0.10 m/s
    Added to the noise model to absorb excess RV scatter; affects significance of the small-amplitude Keplerian signals.
  • Limb-darkening coefficients q1 and q2 = TESS: q1=0.27±0.08, q2=0.22; CHEOPS: q1=0.45, q2=0.32
    Fitted with Gaussian priors from theoretical values; affect transit depth and radius estimates.
assumptions (4)
  • domain assumption The Doppler signals at 4.2, 13.1, and 204.6 d are Keplerian reflex motion from planets, not stellar activity or instrumental artifacts.
    Supported by FAP<0.1%, pre-whitening, and absence of counterparts in log R'HK, BIS, and FWHM periodograms (Sects. 4 and 9), but not directly proven for non-transiting planets c and e.
  • domain assumption The detected transit signals (25.5 d and 4.2 d) are caused by planets transiting TOI-1203 and not by a blended eclipsing binary.
    SOAR speckle imaging rules out companions within 3 arcsec (Sect. 7); TESS centroid tests and CHEOPS follow-up support this (Sects. 2 and 6).
  • domain assumption Stellar parameters (T_eff=5737 K, [Fe/H]=-0.39, R*=1.179 R_sun, M*=0.886 M_sun, age=12.5 Gyr) derived from spectroscopy, photometry, and isochrones are accurate.
    Used in the joint fit to convert RV semi-amplitudes and transit depths into masses and radii (Sects. 8 and 9); independent SME analysis agrees.
  • domain assumption The 613-629 day signal in HARPS CCF FWHM and Th-Ar line widths is instrumental and does not affect the RVs.
    Argued in Sect. 4 from the lack of an RV counterpart and the correspondence with Th-Ar line FWHM, but the physical mechanism is not identified.

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Pith. "Pith review of A four-planet system orbiting the old thick disk star TOI-1203." pith.science (2026). https://pith.science/paper/UFXVYMXB

@misc{pith2026250910136,
  author       = {Pith},
  title        = {Pith review of: A four-planet system orbiting the old thick disk star TOI-1203},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UFXVYMXB}},
  note         = {Machine review of arXiv:2509.10136}
}
abstract

TOI-1203 is a bright (V=8.6) G3 V star known to host a transiting warm sub-Neptune on a 25.5 d orbit. Here we report on an intensive high-precision radial velocity and photometric follow-up campaign carried out with the HARPS spectrograph and the CHEOPS space telescope. We found that TOI-1203 has an enhancement of $\alpha$ elements relative to iron of [$\alpha$/Fe]=$0.21\pm0.04$. With an age of $\sim$12.5 Gyr, TOI-1203 belongs to the old, $\alpha$-element enhanced stellar population of the galactic thick disk. We spectroscopically confirmed the planetary nature of the 25.5 d sub-Neptune TOI-1203 d, measured its mass ($M_{d}=7.39\pm0.62~M_{\oplus}$) and refined its radius ($R_{d}=2.918_{-0.045}^{+0.046}~R_{\oplus}$). We discovered the presence of an additional transiting super-Earth on a 4.2 d orbit (TOI-1203 b) with a mass of $M_{b}=3.51_{-0.32}^{+0.33}~M_{\oplus}$ and a radius of $R_{b}=1.520_{-0.046}^{+0.045}~R_{\oplus}$. We also revealed the presence of two additional low-mass planets at 13.1 d and 204.6 d (TOI-1203 c and e), with minimum masses of $5.46_{-0.50}^{+0.51}~M_{\oplus}$ and $42.10_{-1.78}^{+1.83}~M_{\oplus}$. We found that the outer planet TOI-1203 e lies on an eccentric orbit with $e_{e}=0.152\pm0.029$. We performed a stability analysis of the system confirming that there are configurations consistent with the observed parameters that are dynamically stable over billion-year timescales. While analyzing the HARPS time series, we discovered that the FWHM of the HARPS cross-correlation function shows a significant long-period signal ($\sim$615 d) that has no counterpart in the radial velocity data or in the remaining HARPS ancillary time series. We significantly detected the same signal in the FWHM of the Th-Ar calibration lines used to compute the nightly wavelength solution, and attributed this systematic effect to a long-term variation of the HARPS instrumental profile.

Figures

Figures reproduced from arXiv: 2509.10136 by the authors.

Figure 1
Figure 1. TESS Sector 9 (upper panel), Sector 10 (second panel), Sector 36 (third panel), Sector 63 (fourth panel), and Sector 90 (lower panel) PDC-SAP light curves of TOI-1203. The 120-second data points are displayed as light gray circles, along with the out-of-transit Gaussian process model overplotted in red. The resulting detrended light curves are depicted as blue circles. The transit mid-times of TOI-1203 b and d are m… view at source ↗
Figure 2
Figure 2. Generalized Lomb-Scargle periodograms of the TOI-1203’s HARPS TERRA RVs (upper panel) and of the RV residuals after subtracting the Doppler reflex motion(s) induced by TOI-1203 e (second panel), TOI-1203 e and d (third panel), TOI-1203 e, d, and b (fourth panel), TOI-1203 e, d, b, and c (bottom panel). The dashed horizontal red lines mark the 0.1 % false alarm probability (FAP) as computed using the bootstrap method… view at source ↗
Figure 3
Figure 3. Frequency analysis of the activity indicator and line profile diagnostics of TOI-1203 extracted from the HARPS spectra. Top: Generalized Lomb-Scargle periodograms of: (1) the Ca ii H & K lines activity indicator log R′ HK (upper panel); (2) the bisector inverse slope (BIS) of the HARPS CCF (second panel); (3) the full width at half maximum (FWHM) of the HARPS CCF (lower panel). The dashed horizontal red lines mark t… view at source ↗
Figures from the paper (15 more)
Figure 4
Figure 4. Figure 4: Upper panel: Generalized Lomb-Scargle periodogram of the intensity-weighted average of the FWHM of the Th-Ar spectral lines. The GLS power of the FAP at 0.1 % is marked with a dashed horizontal red line. The dominant signal is found at 0.00159 d−1 (∼629 d). The dashed …
Figure 5
Figure 5. Figure 5: TESS Sector 90 PDC-SAP light curve of TOI-1203. The 120 s data points are displayed with light gray circles, along with the 30-minute binned photometry (black circles). The mid-time of the expected transit of TOI-1203 e, as predicted from the orbital period and referen…
Figure 6
Figure 6. Figure 6: Contrast curve computed from the high-resolution speckle ob￾servations in Cousins I-band on the 4.1 m Southern Astrophysical Re￾search telescope. The inset shows the speckle autocorrelation function centered on the target star. No bright companions are detected within …
Figure 7
Figure 7. Figure 7: Folded transit light curves of TOI-1203 b (left panel) and TOI-1203 d (right panel). The TESS (top) and CHEOPS (bottom) data points are plotted with gray circles. The 20-minute binned photometry is displayed as green and red circles for TESS and CHEOPS, respectively. T…
Figure 8
Figure 8. Figure 8: Upper panel: HARPS TERRA RV time series. The thick black line marks the Keplerian model derived from the medians of the marginalized posterior distributions of the RV parameters (Table B.2). Lower panels: Phase-folded RV curve of TOI-1203 b (middle left), c (middle rig…
Figure 9
Figure 9. Figure 9: Stability analysis of the TOI-1203 system in the orbital period-eccentricity domain: planet b (top left), c (top right), d (bottom left), and e (bottom right). For fixed initial conditions, the phase space of the system is explored by varying the orbital period Pi and …
Figure 10
Figure 10. Figure 10: Evolution of the angle ϖc−ϖd in the TOI-1203 system, starting with the orbital solution listed in Tables B.2 and B.3. 0 0 0 0 0 0   000 00 00 [PITH_FULL_IMAGE:figures/full_fig_p014_10.png]
Figure 11
Figure 11. Figure 11: displays the evolution of the eccentricities and in￾clinations with respect to the invariant plane of the planets over 50 kyr. The inner three planets exhibit considerable variations 0 0 0 0 0 0  00  0 0 0 00 ϖ [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]
Figure 12
Figure 12. Figure 12: Secular evolution of the impact parameter b for TOI-1203 b (blue) and TOI-1203 d (green), starting with the orbital solution listed in Tables B.2 and B.3. 10.2. Resonant chain A three-planet MMR occurs when there exist integers k1, k2, and k3 such that k1n1 + k2n2 + k…
Figure 13
Figure 13. Figure 13: Stability analysis of the TOI-1203 system in the (P12, P23) plane, where P12 = Pc/Pb and P23 = Pc/Pd. For fixed initial condi￾tions, the phase space is explored by varying the period ratios of the inner three planets, while all other parameters are kept at their nom￾i…
Figure 14
Figure 14. Figure 14: Stability analysis of the TOI-1203 system in the (Ω, i) plane for planets c and e, where Ω and i represent the longitude of ascend￾ing node and inclination of each planet, respectively. For each planet, the phase space is explored by varying these two parameters, whil…
Figure 15
Figure 15. Figure 15: Possible location of an additional fifth planet in the TOI-1203 system. The stability of an Earth-size planet (K = 0.1 m s−1 ) is analyzed for various semimajor axes vs. eccentricity. All the angles of the additional fifth planet are set to 0◦ , except for the inclina…
Figure 16
Figure 16. Figure 16: Posterior distributions for the inferred internal structure of TOI-1203 b. Shown are the mass fractions of the inner core (wcore), mantle (wmantle), and envelope (wenvelope), as well as the mass fraction of hydrogen and helium in the volatile layer (1 − Zenvelope), wh…
Figure 17
Figure 17. Figure 17: Same as [PITH_FULL_IMAGE:figures/full_fig_p018_17.png]
Figure 18
Figure 18. Figure 18: Mass-radius diagram for small planets (1 ≤ Rp ≤ 3.5 R⊕, 1 ≤ Mp < 10 M⊕) with mass and radius determinations better than 10 %, as retrieved from the Transiting Extrasolar Planet Catalogue (TEPCat, Southworth 2011, as of July 2025). TOI-1203 b and d are highlighted with…

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Works this paper leans on

156 extracted references · 1 linked inside Pith · cited by 1 Pith paper

  1. [1]

    G., et al

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

    2021

  2. [2]

    C., et al

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

    2015

  3. [3]

    Z., Sousa , S

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

    2012

  4. [4]

    2014, in Exploring the Formation and Evolution of Planetary Systems, ed

    Allard , F. 2014, in Exploring the Formation and Evolution of Planetary Systems, ed. M. Booth , B. C. Matthews , & J. R. Graham , Vol. 299, 271--272

    2014

  5. [5]

    M., et al

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

    2024

  6. [6]

    W., & O'Neil , M

    Ambikasaran , S., Foreman-Mackey , D., Greengard , L., Hogg , D. W., & O'Neil , M. 2015, IEEE Transactions on Pattern Analysis and Machine Intelligence, 38, 252

    2015

  7. [7]

    R., Collier Cameron , A., Hellier , C., et al

    Anderson , D. R., Collier Cameron , A., Hellier , C., et al. 2011, , 726, L19

    2011

  8. [8]

    J., Barnes , J., et al

    Anglada-Escud \'e , G., Amado , P. J., Barnes , J., et al. 2016, , 536, 437

    2016

Show all 156 references
  1. [9]

    & Butler , R

    Anglada-Escud \'e , G. & Butler , R. P. 2012, , 200, 15

    2012

  2. [10]

    2015, , 450, 1787

    Angus , R., Aigrain , S., Foreman-Mackey , D., & McQuillan , A. 2015, , 450, 1787

    2015

  3. [11]

    1994, , 291, 895

    Axer , M., Fuhrmann , K., & Gehren , T. 1994, , 291, 895

    1994

  4. [12]

    1996, , 119, 373

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

    1996

  5. [13]

    Barnes , S. A. 2007, , 669, 1167

    2007

  6. [14]

    M., & Zicher , N

    Barrag \'a n , O., Aigrain , S., Rajpaul , V. M., & Zicher , N. 2021,

    2021

  7. [15]

    J., Gandolfi , D., et al

    Barrag \'a n , O., Armstrong , D. J., Gandolfi , D., et al. 2022, , 514, 1606

    2022

  8. [16]

    2019, , 482, 1017

    Barrag \'a n , O., Gandolfi , D., & Antoniciello , G. 2019, , 482, 1017

    2019

  9. [17]

    2021, Experimental Astronomy, 51, 109

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

    2021

  10. [18]

    Blackwell , D. E. & Shallis , M. J. 1977, , 180, 177

    1977

  11. [19]

    J., et al

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

    2021

  12. [20]

    A., et al

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

    2023

  13. [21]

    2016, , 585, A5

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

    2016

  14. [22]

    2015, , 575, A18

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

    2015

  15. [23]

    J., Koch , D., Basri , G., et al

    Borucki , W. J., Koch , D., Basri , G., et al. 2010, Science, 327, 977

    2010

  16. [24]

    2009, , 496, 527

    Bouchy , F., Mayor , M., Lovis , C., et al. 2009, , 496, 527

    2009

  17. [25]

    A., & Morris , B

    Brandeker , A., Patel , J. A., & Morris , B. M. 2024, PIPE: Extracting PSF photometry from CHEOPS data , Astrophysics Source Code Library, record ascl:2404.002

    2024

  18. [26]

    R., Quirion , P

    Bruntt , H., Bedding , T. R., Quirion , P. O., et al. 2010, , 405, 1907

    2010

  19. [27]

    2012, , 548, A44

    Cabrera , J., Csizmadia , S., Erikson , A., Rauer , H., & Kirste , S. 2012, , 548, A44

    2012

  20. [28]

    M., et al

    Cabrera , J., Gandolfi , D., Serrano , L. M., et al. 2023, , 675, A183

    2023

  21. [29]

    2020, , 160, 114

    Carleo , I., Gandolfi , D., Barrag \'a n , O., et al. 2020, , 160, 114

    2020

  22. [30]

    & Kurucz , R

    Castelli , F. & Kurucz , R. L. 2003, in IAU Symposium, Vol. 210, Modelling of Stellar Atmospheres, ed. N. Piskunov , W. W. Weiss , & D. F. Gray , A20

    2003

  23. [31]

    2017, , 600, A30

    Claret , A. 2017, , 600, A30

    2017

  24. [32]

    2021, Research Notes of the American Astronomical Society, 5, 13

    Claret , A. 2021, Research Notes of the American Astronomical Society, 5, 13

    2021

  25. [33]

    Correia , A. C. M., Couetdic, J., Laskar, J., et al. 2010,

    2010

  26. [34]

    Correia , A. C. M., Udry , S., Mayor , M., et al. 2005, , 440, 751

    2005

  27. [35]

    Couetdic , J., Laskar , J., Correia , A. C. M., Mayor , M., & Udry , S. 2010,

    2010

  28. [36]

    Delisle , J. B. & Laskar , J. 2014, , 570, L7

    2014

  29. [37]

    B., Laskar , J., & Correia , A

    Delisle , J. B., Laskar , J., & Correia , A. C. M. 2014, , 566, A137

    2014

  30. [38]

    B., Laskar , J., Correia , A

    Delisle , J. B., Laskar , J., Correia , A. C. M., & Bou \'e , G. 2012, , 546, A71

    2012

  31. [39]

    Demangeon , O. D. S., Zapatero Osorio , M. R., Alibert , Y., et al. 2021, , 653, A41

    2021

  32. [40]

    P., Davies , G

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

    2014

  33. [41]

    2011, , 535, A55

    Dumusque , X., Lovis , C., S \'e gransan , D., et al. 2011, , 535, A55

    2011

  34. [42]

    Eastman , J., Siverd , R., & Gaudi , B. S. 2010, , 122, 935

    2010

  35. [43]

    A., Osborn , H

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

    2024

  36. [44]

    J., Gandolfi , D., et al

    Esposito , M., Armstrong , D. J., Gandolfi , D., et al. 2019, , 623, A165

    2019

  37. [45]

    2013, Celes

    Farr \'e s , A., Laskar , J., Blanes , S., et al. 2013, Celes. Mech. Dyn. Astron., 116, 141

    2013

  38. [46]

    D., Montet , B

    Feinstein , A. D., Montet , B. T., Foreman-Mackey , D., et al. 2019, , 131, 094502

    2019

  39. [47]

    2014, george: George (v0.2.0)

    Foreman-Mackey , D., Hoyer , S., Bernhard , J., & Angus , R. 2014, george: George (v0.2.0)

    2014

  40. [48]

    E., Broeg , C., et al

    Fortier , A., Simon , A. E., Broeg , C., et al. 2024, , 687, A302

    2024

  41. [49]

    2020, , 498, 4503

    Fridlund , M., Livingston , J., Gandolfi , D., et al. 2020, , 498, 4503

    2020

  42. [50]

    1993, , 271, 451

    Fuhrmann , K., Axer , M., & Gehren , T. 1993, , 271, 451

    1993

  43. [51]

    1994, , 285, 585

    Fuhrmann , K., Axer , M., & Gehren , T. 1994, , 285, 585

    1994

  44. [52]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1

    2023

  45. [53]

    P., et al

    Gandolfi , D., Barrag \'a n , O., Hatzes , A. P., et al. 2017, , 154, 123

    2017

  46. [54]

    H., et al

    Gandolfi , D., Barrag \'a n , O., Livingston , J. H., et al. 2018, , 619, L10

    2018

  47. [55]

    Y., Persson , C

    Georgieva , I. Y., Persson , C. M., Goffo , E., et al. 2023, , 674, A117

    2023

  48. [56]

    D., Jensen , E

    Giacalone , S., Dressing , C. D., Jensen , E. L. N., et al. 2021, , 161, 24

    2021

  49. [57]

    2024, , 685, A147

    Goffo , E., Chaturvedi , P., Murgas , F., et al. 2024, , 685, A147

    2024

  50. [58]

    A., et al

    Goffo , E., Gandolfi , D., Egger , J. A., et al. 2023, , 955, L3

    2023

  51. [59]

    M., Seager , S., Huang , C

    Guerrero , N. M., Seager , S., Huang , C. X., et al. 2021, , 254, 39

    2021

  52. [60]

    2008, , 486, 951

    Gustafsson , B., Edvardsson , B., Eriksson , K., et al. 2008, , 486, 951

    2008

  53. [61]

    2024, , 681, A96

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

    2024

  54. [62]

    D., Bakos , G

    Hartman , J. D., Bakos , G. \'A ., Bouma , L. G., & Csubry , Z. 2025, , 137, 024501

    2025

  55. [63]

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

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

    2010

  56. [64]

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

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

    2022

  57. [65]

    J., et al

    Hoyer , S., Gandolfi , D., Armstrong , D. J., et al. 2021, , 505, 3361

    2021

  58. [66]

    2020, , 635, A24

    Hoyer , S., Guterman , P., Demangeon , O., et al. 2020, , 635, A24

    2020

  59. [67]

    Jenkins , J. M. 2002, , 575, 493

    2002

  60. [68]

    M., Chandrasekaran , H., McCauliff , S

    Jenkins , J. M., Chandrasekaran , H., McCauliff , S. D., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7740, Software and Cyberinfrastructure for Astronomy, ed. N. M. Radziwill & A. Bridger , 77400D

    2010

  61. [69]

    M., Tenenbaum , P., Seader , S., et al

    Jenkins , J. M., Tenenbaum , P., Seader , S., et al. 2020, Kepler Data Processing Handbook: Transiting Planet Search , Kepler Science Document KSCI-19081-003, id. 9. Edited by Jon M. Jenkins

    2020

  62. [70]

    M., Twicken , J

    Jenkins , J. M., Twicken , J. D., McCauliff , S., et al. 2016, in , Vol. 9913, Software and Cyberinfrastructure for Astronomy IV, 99133E

    2016

  63. [71]

    Kipping , D. M. 2013, , 435, 2152

    2013

  64. [72]

    2023, , 519, 5637

    Knudstrup , E., Gandolfi , D., Nowak , G., et al. 2023, , 519, 5637

    2023

  65. [73]

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

    1997

  66. [74]

    Kurucz , R. L. 1993 a , SYNTHE spectrum synthesis programs and line data

    1993

  67. [75]

    Kurucz , R. L. 1993 b , SYNTHE spectrum synthesis programs and line data (Astrophysics Source Code Library)

    1993

  68. [76]

    1990, , 88, 266

    Laskar , J. 1990, , 88, 266

    1990

  69. [77]

    1993, Physica D: Nonlinear Phenomena

    Laskar, J. 1993, Physica D: Nonlinear Phenomena

    1993

  70. [78]

    D., et al

    Li , J., Tenenbaum , P., Twicken , J. D., et al. 2019, , 131, 024506

    2019

  71. [79]

    J., et al

    Lillo-Box , J., Gandolfi , D., Armstrong , D. J., et al. 2023, , 669, A109

    2023

  72. [80]

    2021, , 649, A4

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

    2021

  73. [81]

    J., Ragozzine , D., Fabrycky , D

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

    2011

  74. [82]

    2013, , 551, A59

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

    2013

  75. [83]

    Lomb , N. R. 1976, , 39, 447

    1976

  76. [84]

    & Pepe , F

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

    2007

  77. [85]

    2011, , 528, A112

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

    2011

  78. [86]

    N., Handberg , R., Buzasi , D

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

    2021

  79. [87]

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

    2008

  80. [88]

    & Agol , E

    Mandel , K. & Agol , E. 2002, , 580, L171

    2002

  81. [89]

    2024 a , , 682, A129

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

    2024

  82. [90]

    G., Borsato , L., et al

    Mantovan , G., Wilson , T. G., Borsato , L., et al. 2024 b , , 691, A67

    2024

  83. [91]

    2017, , 835, 77

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

    2017

  84. [92]

    Maxted , P. F. L., Anderson , D. R., Collier Cameron , A., et al. 2011, , 123, 547

    2011

  85. [93]

    Maxted , P. F. L., Ehrenreich , D., Wilson , T. G., et al. 2023, pycheops: Light curve analysis for ESA CHEOPS data , Astrophysics Source Code Library, record ascl:2312.034

    2023

  86. [94]

    2003, The Messenger, 114, 20

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

    2003

  87. [95]

    Mermilliod , J. C. 1987, , 71, 413

    1987

  88. [96]

    L., Twicken , J

    Morris , R. L., Twicken , J. D., Smith , J. C., et al. 2020, Kepler Data Processing Handbook: Photometric Analysis , Kepler Science Document KSCI-19081-003

    2020

  89. [97]

    R., Malavolta , L., et al

    Mortier , A., Zapatero Osorio , M. R., Malavolta , L., et al. 2020, , 499, 5004

    2020

  90. [98]

    & Michel , K.-U

    Mugrauer , M. & Michel , K.-U. 2020, Astronomische Nachrichten, 341, 996

    2020

  91. [99]

    A., Hearnshaw , J

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

    1993

  92. [100]

    R., Bergemann , M., Eitner , P., & Johansen , A

    Nielsen , J., Gent , M. R., Bergemann , M., Eitner , P., & Johansen , A. 2023, , 678, A74

    2023

  93. [101]

    D., Gandolfi , D., Armstrong , D

    Nielsen , L. D., Gandolfi , D., Armstrong , D. J., et al. 2020, , 492, 5399

    2020

  94. [102]

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

    2024

  95. [103]

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

    Otegi , J. F., Bouchy , F., & Helled , R. 2020, , 634, A43

    2020

  96. [104]

    Pecaut , M. J. & Mamajek , E. E. 2013, , 208, 9

    2013

  97. [105]

    J., Mamajek , E

    Pecaut , M. J., Mamajek , E. E., & Bubar , E. J. 2012, , 746, 154

    2012

  98. [106]

    2021, , 645, A96

    Pepe , F., Cristiani , S., Rebolo , R., et al. 2021, , 645, A96

    2021

  99. [107]

    2002, , 388, 632

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

    2002

  100. [108]

    2004, , 423, 385

    Pepe , F., Mayor , M., Queloz , D., et al. 2004, , 423, 385

    2004

  101. [109]

    M., Georgieva , I

    Persson , C. M., Georgieva , I. Y., Gandolfi , D., et al. 2022, , 666, A184

    2022

  102. [110]

    & Valenti , J

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

    2017

  103. [111]

    L., Skillen , I., Collier Cameron , A., et al

    Pollacco , D. L., Skillen , I., Collier Cameron , A., et al. 2006, , 118, 1407

    2006

  104. [112]

    E., Lambert , D

    Reddy , B. E., Lambert , D. L., & Allende Prieto , C. 2006, , 367, 1329

    2006

  105. [113]

    R., Winn , J

    Ricker , G. R., Winn , J. N., Vanderspek , R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003

    2015

  106. [114]

    Salmon , S. J. A. J., Van Grootel , V., Buldgen , G., Dupret , M. A., & Eggenberger , P. 2021, , 646, A7

    2021

  107. [115]

    C., Adibekyan , V., Dorn , C., et al

    Santos , N. C., Adibekyan , V., Dorn , C., et al. 2017, , 608, A94

    2017

  108. [116]

    C., Sousa , S

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

    2013

  109. [117]

    Scargle , J. D. 1982, , 263, 835

    1982

  110. [118]

    2020, , 499, 428

    Schanche , N., H \'e brard , G., Collier Cameron , A., et al. 2020, , 499, 428

    2020

  111. [119]

    2010, , 403, 1829

    Sch \"o nrich , R., Binney , J., & Dehnen , W. 2010, , 403, 1829

    2010

  112. [120]

    2008, , 316, 83

    Scuflaire , R., Th \'e ado , S., Montalb \'a n , J., et al. 2008, , 316, 83

    2008

  113. [121]

    2023, , 524, 5781

    See , V., Roquette , J., Amard , L., & Matt , S. 2023, , 524, 5781

    2023

  114. [122]

    See , V., Roquette , J., Amard , L., & Matt , S. P. 2021, , 912, 127

    2021

  115. [123]

    M., Gandolfi , D., Mustill , A

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

    2022

  116. [124]

    F., Cutri , R

    Skrutskie , M. F., Cutri , R. M., Stiening , R., et al. 2006, , 131, 1163

    2006

  117. [125]

    C., Stumpe , M

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

    2012

  118. [126]

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

    1973

  119. [127]

    Sousa , S. G. 2014, [arXiv:1407.5817] [ [arXiv] 1407.5817 ]

    2014 arXiv

  120. [128]

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

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

    2021

  121. [129]

    G., Santos , N

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

    2015

  122. [130]

    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

  123. [131]

    G., Santos , N

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

    2008

  124. [132]

    2011, , 417, 2166

    Southworth , J. 2011, , 417, 2166

    2011

  125. [133]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Pepper , J., et al. 2018, , 156, 102

    2018

  126. [134]

    C., Smith , J

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

    2014

  127. [135]

    C., Smith , J

    Stumpe , M. C., Smith , J. C., Van Cleve , J. E., et al. 2012, , 124, 985

    2012

  128. [136]

    I., & Esposito , M

    Su \'a rez Mascare \ n o , A., Rebolo , R., Gonz \'a lez Hern \'a ndez , J. I., & Esposito , M. 2015, , 452, 2745

    2015

  129. [137]

    L., Berger , T

    Sullivan , K., Kraus , A. L., Berger , T. A., et al. 2024, , 168, 129

    2024

  130. [138]

    2015, , 580, A30

    Thiabaud , A., Marboeuf , U., Alibert , Y., Leya , I., & Mezger , K. 2015, , 580, A30

    2015

  131. [139]

    2018, , 130, 035002

    Tokovinin , A. 2018, , 130, 035002

    2018

  132. [140]

    2007, , 378, 72

    Trotta , R. 2007, , 378, 72

    2007

  133. [141]

    D., Catanzarite , J

    Twicken , J. D., Catanzarite , J. H., Clarke , B. D., et al. 2018, , 130, 064502

    2018

  134. [142]

    D., Chandrasekaran , H., Jenkins , J

    Twicken , J. D., Chandrasekaran , H., Jenkins , J. M., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7740, Software and Cyberinfrastructure for Astronomy, ed. N. M. Radziwill & A. Bridger , 77401U

    2010

  135. [143]

    2019, , 622, A37

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

    2019

  136. [144]

    A., Butler , R

    Valenti , J. A., Butler , R. P., & Marcy , G. W. 1995, , 107, 966

    1995

  137. [145]

    Valenti , J. A. & Piskunov , N. 1996, , 118, 595

    1996

  138. [146]

    2021, , 507, 2154

    Van Eylen , V., Astudillo-Defru , N., Bonfils , X., et al. 2021, , 507, 2154

    2021

  139. [147]

    2025, , 693, A235

    S ubjak , J., Gandolfi , D., Goffo , E., et al. 2025, , 693, A235

    2025

  140. [148]

    2025, , 539, 405

    Weeks , A., Van Eylen , V., Huber , D., et al. 2025, , 539, 405

    2025

  141. [149]

    G., Goffo , E., Alibert , Y., et al

    Wilson , T. G., Goffo , E., Alibert , Y., et al. 2022, , 511, 1043

    2022

  142. [150]

    Winn , J. N. 2010, in Exoplanets, ed. S. Seager , 55--77

    2010

  143. [151]

    L., Eisenhardt , P

    Wright , E. L., Eisenhardt , P. R. M., Mainzer , A. K., et al. 2010, , 140, 1868

    2010

  144. [152]

    2001, , 136, 417

    Yi , S., Demarque , P., Kim , Y.-C., et al. 2001, , 136, 417

    2001

  145. [153]

    & K \"u rster , M

    Zechmeister , M. & K \"u rster , M. 2009, , 496, 577

    2009

  146. [154]

    2020, , 159, 19

    Ziegler , C., Tokovinin , A., Brice \ n o , C., et al. 2020, , 159, 19

    2020

  147. [155]

    , " * 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...

  148. [156]

    write newline

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Pith tools

Reviewed August 4, 2026 · model on record in the stance chip above.