Pith. sign in

REVIEW 6 minor 136 references

The mass of TOI-654 b: A short-period sub-Neptune transiting a mid-M dwarf

T0 review · 0 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read TOI-654 b, a 1.53-day sub-Neptune around a mid-M dwarf, is measured to have 8.71 Earth masses and an updated radius of 2.378 Earth radii.

desk verdict A clean, standard RV+transit measurement that gives TOI-654 b its first direct mass; worth a serious referee, with data-release as the main condition. read the letter →

arxiv 2507.16222 v1 pith:RJSZPP43 submitted 2025-07-22 astro-ph.EP astro-ph.SR

Kai Ikuta , Norio Narita , Takuya Takarada , Teruyuki Hirano , Akihiko Fukui , Hiroyuki Tako Ishikawa , Yasunori Hori , Tadahiro Kimura
show 35 more authors
Takanori Kodama Masahiro Ikoma Jerome P. de Leon Kiyoe Kawauchi Masayuki Kuzuhara Gaia Lacedelli John H. Livingston Mayuko Mori Felipe Murgas Enric Palle Hannu Parviainen Noriharu Watanabe Izuru Fukuda Hiroki Harakawa Yuya Hayashi Klaus Hodapp Keisuke Isogai Taiki Kagetani Yugo Kawai Vigneshwaran Krishnamurthy Tomoyuki Kudo Takashi Kurokawa Nobuhiko Kusakabe Jun Nishikawa Stevanus K. Nugroho Masashi Omiya Takuma Serizawa Aoi Takahashi Huan-Yu Teng Yuka Terada Akitoshi Ueda Sébastien Vievard Yujie Zou Takayuki Kotani Motohide Tamura
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords sub-NeptuneexoplanetmassmeasurementradialvelocitytransitphotometryMdwarfradiusvalleyNeptunedesertplanetcomposition
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

TOI-654 b is a 1.53-day sub-Neptune transiting a mid-M dwarf, and this paper sets its mass rather than relying on a radius-only estimate. Using Subaru/IRD radial velocities plus TESS and MuSCAT transit photometry, the authors report $M_p = 8.71 \pm 1.25 M_\oplus$ and an updated $R_p = 2.378 \pm 0.089 R_\oplus$. The implied mean density of $3.59 \pm 0.65$ g cm$^{-3}$ is high enough to exclude a substantial hydrogen envelope, yet it leaves two compositions open: a rocky core with a thin H/He layer or a volatile-rich water core. Because TOI-654 b sits near the M-dwarf radius valley and on the outer edge of the Neptune desert, a precise mass here helps decide which formation and loss mechanisms carve out those regions.

What carries the argument

The load-bearing measurement is the radial-velocity semi-amplitude $K = 8.62^{+1.22}_{-1.23}$ m s$^{-1}$ extracted from 85 Subaru/IRD spectra, combined in a joint transit-plus-RV model and sampled with a Hamiltonian Monte Carlo scheme. The transit side uses TESS photometry from six sectors and ground-based MuSCAT2/MuSCAT3 multicolor light curves, with a Matérn-3/2 Gaussian-process baseline (a smooth, time-correlated noise model) for the ground-based data. Stellar mass and radius come from empirical mass-luminosity and radius-luminosity relations plus spectral energy distribution fitting, giving $M_s = 0.419 \pm 0.009 M_\odot$ and $R_s = 0.430 \pm 0.013 R_\odot$; since $M_p \propto M_s^{2/3}$ and $R_p \propto R_s$, these stellar calibrations directly set the headline planetary values.

What would settle it

A direct measurement of the stellar angular diameter by long-baseline interferometry, or an asteroseismic radius that contradicts $R_s = 0.430 \pm 0.013 R_\odot$, would rescale the planet's radius linearly; likewise, a larger independent RV dataset that moved $K$ outside $8.62^{+1.22}_{-1.23}$ m s$^{-1}$ would change the mass. If either measurement pushed the derived density outside $3.59 \pm 0.65$ g cm$^{-3}$, the composition interpretation would need revision.

Watch

Extended reading notes

Core claim

The central result is a measured planetary mass of $M_p = 8.71 \pm 1.25 M_\oplus$ and an updated radius of $R_p = 2.378 \pm 0.089 R_\oplus$ from a joint fit of the transit light curves and the IRD radial velocities, with the circular-orbit model favored slightly over an eccentric one ($\Delta \log Z = 0.158$). The paper reports that the resulting bulk density, $\rho_p = 3.59 \pm 0.65$ g cm$^{-3}$, places TOI-654 b equally close to a rocky core plus roughly 0.3 wt\% hydrogen envelope and to a 50 wt\% rock / 50 wt\% water composition under the relevant temperature. The radius precision improves from 5.3\% to 3.7\% relative to the earlier validation, and the updated Transmission and Emission Spectroscopy Metrics (TSM $= 49 \pm 8$, ESM $= 11 \pm 1$) make the planet a viable emission-spectroscopy target for JWST and Ariel, though not a strong transmission-spectroscopy target.

Load-bearing premise

The adopted stellar mass and radius come from empirical brightness-to-size relations rather than direct measurement, so a systematic error there would shift the planet's mass and radius in lockstep.

Editorial extensions

If this is right

  • TOI-654 b's density of $3.59 \pm 0.65$ g cm$^{-3}$ excludes a purely hydrogen-dominated sub-Neptune and restricts any H/He envelope to a small fraction of the planet's mass.
  • At $P = 1.53$ days and $R_p = 2.378 R_\oplus$, the planet sits near the M-dwarf radius valley and on the outer edge of the Neptune desert, so its measured mass anchors both population features around a single object.
  • The improved stellar radius shrinks the planetary radius uncertainty from 5.3\% to 3.7\%, tightening the target list for JWST and Ariel emission spectroscopy.
  • The updated TSM and ESM values ($49 \pm 8$ and $11 \pm 1$) show the planet is better suited to secondary-eclipse emission observations than to transmission spectroscopy.

Reading between the lines

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

  • If the mass holds up, TOI-654 b becomes a useful discriminator for M-dwarf radius-valley models: a dense, sub-Neptune-sized planet close to the valley is more naturally explained by photoevaporative stripping of a primordial envelope than by gas-poor formation, though the paper does not choose between these.
  • A single JWST emission spectrum, or one more transit observed in transmission, could break the rock-plus-envelope versus water-world degeneracy that the current density cannot resolve; this is the paper's own suggested next step and is within reach.
  • The He I 1083 nm data taken during the MuSCAT3 transit, reported in a forthcoming companion paper, may connect atmospheric escape to the planet's position in the Neptune desert, but that connection is not established here.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

0 major / 6 minor

Summary. The paper reports follow-up characterization of the transiting sub-Neptune TOI-654 b (P = 1.528 d) around a mid-M dwarf. Using TESS and MuSCAT2/MuSCAT3 photometry combined with 85 Subaru/IRD radial-velocity measurements, the authors perform a joint transit+RV fit and derive a planet mass of 8.71 ± 1.25 M_Earth from a 7σ semi-amplitude K = 8.62 ± 1.22 m/s, an updated radius of 2.378 ± 0.089 R_Earth, and a mean density of 3.59 ± 0.65 g/cm3. Stellar parameters are obtained from empirical mass/radius-luminosity relations and an SED fit; activity indicators show no significant signal at the planet period, and a circular orbit is favored over an eccentric one by ΔlnZ = 0.158. The paper discusses the resulting composition degeneracy (rocky core + H/He envelope vs. water-rich), the planet's position near the radius valley and the Neptune desert, and its potential for JWST/Ariel follow-up.

Significance. This is a useful addition to the small sample of M-dwarf sub-Neptunes with precisely measured masses and radii. The RV detection is robust (K = 8.62 ± 1.22 m/s, FAP < 0.1%), the activity analysis is careful, and the circular/eccentric model comparison gives consistent masses, so the central claim is well supported. The paper uses public modeling tools (jaxoplanet, tinygp, emcee, NumPyro) and explicitly reports a model-evidence comparison. I find no circularity: the mass comes from the RV semi-amplitude and an independently adopted stellar mass, not from the same data used to derive the transit parameters. The main limitation is that the adopted stellar radius and mass inherit possible systematics from empirical relations, but the SED-based radius is consistent, and the impact on M_p is small (M_p ∝ M_s^(2/3)). Overall, the paper delivers a solid, timely characterization.

minor comments (6)
  1. [3.1.2 / Table 1] The SED-derived radius (0.422+0.011/−0.009 R_sun) is statistically consistent with the adopted empirical value (0.430 ± 0.013 R_sun), but the empirical value is chosen without explanation. Please add one sentence justifying this choice, and state whether systematic errors in the Mann et al. mass/radius relations are included in the quoted uncertainties.
  2. [Data availability] The paper does not include a data availability statement or machine-readable tables of the 85 IRD radial velocities and the TESS/MuSCAT2/MuSCAT3 light curves used in the joint fit. Given that the IRD spectra are not public, releasing the derived RVs (and preferably the jaxoplanet model configuration) would greatly aid independent verification.
  3. [Abstract] The abstract contains a duplicated word: 'radius valley and and also on the outer edge'.
  4. [4.1] The phrase 'one of unique planets' should be 'one of the unique planets' or better 'one of a small number of planets'.
  5. [3.2.3] The ΔlnZ value of 0.158 between the circular and eccentric models corresponds to 'not worth more than a bare mention' in the Kass & Raftery (1995) scale. Please state explicitly that the two models are statistically indistinguishable and that the choice of the circular model as the fiducial model does not affect the quoted mass, only the eccentricity-related caveats.
  6. [3.1.2] The explicit caveat that the Teff uncertainty does not include stellar-model systematics is appreciated; consider also noting the potential effect on the limb-darkening priors, even though the adopted 3× wider priors should render it negligible.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the planet mass and radius rest on independent RV, transit, and stellar-calibration inputs, with no load-bearing self-citation or fitted-input-as-prediction step.

full rationale

The derivation chain for the central claim is self-contained and does not reduce to its own inputs. The planetary mass, M_p = 8.71 +/- 1.25 M_earth, is obtained from the measured RV semi-amplitude K = 8.62 +/- 1.22 m/s (GLS FAP < 0.1%) combined with the adopted stellar mass M_s = 0.419 +/- 0.009 M_sun, which is taken from independent empirical mass-luminosity and metallicity relations (Mann et al. 2015, 2019) and cross-checked with an SED fit; the stellar mass is not fit to the RV or transit data. Similarly, the planet radius, R_p = 2.378 +/- 0.089 R_earth, is the product of the transit-derived ratio R_p/R_s = 0.0510 +/- 0.0008 and the independently adopted stellar radius R_s = 0.430 +/- 0.013 R_sun, which also agrees with the SED-derived radius. The circular-orbit choice is not an input that defines the mass: the eccentric model yields a consistent mass (8.87 +/- 1.23 M_earth), and the circular model is preferred only by a negligible Bayesian evidence difference (Delta log Z = 0.158). Activity indicators (FWHM, dV, CRX, dLW) and archival photometry show no significant signal at the 1.528-day period, so the RV signal is not being driven by a fitted activity model. The paper does use several pipelines and reduction procedures from co-authored prior work (IRD extraction, MuSCAT photometry), but those are data-processing tools rather than the theoretical or empirical claim itself; no stated uniqueness theorem or ansatz is imported from a self-citation to force the result. The acknowledged limitations, such as the Teff uncertainty excluding stellar atmospheric model systematics and the lack of released machine-readable data, affect accuracy and reproducibility but do not constitute circularity. Overall, no derivation step equates the prediction with a fitted parameter or with the authors' own prior assertion by construction.

Assumptions & free parameters 8 free parameters · 5 assumptions · 0 invented entities

The central claim rests on standard empirical stellar calibrations, model atmospheres, and noise-model choices, with no new particles, forces, or physical entities introduced.

free parameters (8)
  • K (RV semi-amplitude) = 8.62 +1.22/-1.23 m/s
    Fitted to 85 IRD radial velocities; directly sets the planet mass.
  • Rp/Rs (planet-to-star radius ratio) = 0.0510 ± 0.0008
    Fitted to TESS and MuSCAT transits; combined with the stellar radius gives R_p.
  • impact parameter b = 0.290 +0.104/-0.112
    Fitted to transit shape; affects transit duration, depth, and derived inclination.
  • orbital period P = 1.527561 ± 0.000001 d
    Fitted jointly in the transit and RV models; strongly anchored by many TESS transits.
  • stellar mass M_s = 0.419 ± 0.009 M_sun
    Adopted from an empirical mass-luminosity relation (Mann et al. 2019) rather than directly measured; M_p scales as M_s^(2/3).
  • stellar radius R_s = 0.430 ± 0.013 R_sun
    Adopted from an empirical radius-luminosity relation (Mann et al. 2015) and SED fitting; R_p scales linearly with R_s.
  • limb-darkening coefficients q1, q2 = See Table 4
    Fitted per band with Gaussian priors derived from the PHOENIX model; influence the transit depth and limb shape.
  • jitter and Gaussian-process hyperparameters = See Table 4
    Fitted to absorb photometric and RV correlated noise; part of the noise model rather than the central signal.
assumptions (5)
  • domain assumption Empirical M dwarf mass-luminosity and radius-luminosity relations calibrated on other stars apply to TOI-654.
    Invoked in Section 3.1.2 to set M_s and R_s; errors in these relations propagate into M_p and R_p.
  • domain assumption One-dimensional LTE model atmospheres (MARCS, BT-Settl) adequately represent the stellar spectrum and SED.
    Used in Sections 3.1.1 and 3.1.2 for Teff and abundances; the paper notes an unquantified model-systematic uncertainty.
  • domain assumption The 1.528-day RV signal is planetary rather than stellar activity.
    Supported by a GLS FAP below 0.1% and the absence of significant peaks in FWHM, dV, CRX, dLW, and photometry, but the possibility of M dwarf activity is not fully excluded.
  • domain assumption The orbit is circular for the adopted fiducial parameters.
    Section 3.2.3: ΔlogZ = 0.158 slightly favors circular over eccentric, but the difference is inconclusive by Kass and Raftery criteria; the derived mass differs by only 0.16 M_Earth between models.
  • domain assumption A Matérn-3/2 Gaussian process describes the correlated noise in the ground photometry.
    Equation (1) models time-correlated systematics for MuSCAT2 and MuSCAT3; the specific kernel choice is not independently tested against alternatives.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The mass of TOI-654 b: A short-period sub-Neptune transiting a mid-M dwarf." pith.science (2026). https://pith.science/paper/RJSZPP43

@misc{pith2026250716222,
  author       = {Pith},
  title        = {Pith review of: The mass of TOI-654 b: A short-period sub-Neptune transiting a mid-M dwarf},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RJSZPP43}},
  note         = {Machine review of arXiv:2507.16222}
}
abstract

Sub-Neptunes are small planets between the size of the Earth and Neptune. The orbital and bulk properties of transiting sub-Neptunes can provide clues for their formation and evolution of small planets. In this paper, we report on follow-up observations of a planetary system around the mid-M dwarf TOI-654, whose transiting sub-Neptune TOI-654 b ($P=1.53$ day) is validated as a suitable target for the atmospheric observation. We measure the planetary mass and stellar properties with the InfraRed Doppler instrument (IRD) mounted on the Subaru telescope and obtain the stellar and planetary properties from additional transit observations by the Transit Exoplanetary Survey Satellite (TESS) and a series of the Multicolor Simultaneous Camera for studying Atmospheres of Transiting exoplanets (MuSCAT). As a result, the planetary mass of TOI-654 b is determined to be $M_{{\rm p}} = 8.71 \pm 1.25 M_{\oplus}$, and the radius is updated to be $R_{\rm p} = 2.378 \pm 0.089 R_{\oplus}$. The bulk density suggests that the planet is composed of a rocky and volatile-rich core or a rocky core surrounded by a small amount of H/He envelope.TOI-654 b is one of unique planets located around the radius valley and and also on the outer edge of the Neptune desert. The precise mass determination enables us to constrain the atmospheric properties with future spectroscopic observations especially for the emission by the James Webb Space Telescope and Ariel.

Figures

Figures reproduced from arXiv: 2507.16222 by the authors.

Figure 1
Figure 1. Phase-folded TESS light curve (gray) with the derived orbital period (= 1.528 day) and optimum model (orange) near the transit center within transit windows of three times the transit duration of TOI-654 b (Section 2.1). Alt text: Time-series flux for the transit of the TESS data and the optimum model. and is capable of simultaneous imaging in g-, r-, i-, and zs-bands with a field of view of 9’1 × 9’1. The exposure … view at source ↗
Figure 2
Figure 2. Multicolor simultaneous light curves in g-, r-, i-, and zs-bands, obtained by MuSCAT2 on 2021 March 19 (Top) and MuSCAT3 on 2021 January 28 (Bottom) (Section 2.2 and 2.3). The data are jointly fitted with the transit model (blue, green, orange, and red) and baseline model, and the data are subtracted with the baseline models (gray). Alt text: Time-series flux for the transits of the MuSCAT2 and MuSCAT3 data in g-, r… view at source ↗
Figure 4
Figure 4. Spectrum energy distributions (SED) of TOI-654. Yellow and green curves show the prior and posterior of the SED models. Red diamonds and blue squares are data and optimum, respectively (for details, Section 3.1.2). Alt text: Wavelength (Å) versus flux density (erg cm−2 s −1 Å −1 ) as the SED. Diamond and square show the observed data and optimum point. Two lines show the prior distribution for fitting the SED and th… view at source ↗
Figures from the paper (7 more)
Figure 3
Figure 3. Figure 3: Time-series RV, FWHM, dV, CRX, and dLW (blue) for TOI-654 from the IRD spectra (Section 2.4). Alt text: Time-series RV, FWHM, dV, CRX, and dLW, from the IRD spectra for each panel. the elemental abundances of Na, Mg, Ca, Ti, Cr, Mn, Fe, and Sr, from the corresponding a…
Figure 5
Figure 5. Figure 5: Periodograms of the RV, Window, O-C, FWHM, dV, CRX, and dLW, obtained with the GLS from the IRD spectra for TOI-654 (Section 3.1.3). The horizontal lines represent the FAP of 0.1, 1.0, and 5.0 %, respectively (black) for each of the panel. In the top panel for the RV, …
Figure 6
Figure 6. Figure 6: The phase-folded RV data with the orbital period (= 1.528 day) of the planet TOI-654 b (blue), the circular model with its uncertainty (red), and the residual from the model. Alt text: The orbital phase versus the relative RV (m s−1 ) and residual (m s−1 ). The relativ…
Figure 8
Figure 8. Figure 8: Period-Radius diagram for TOI-654 b (red), TOI-4479 b (blue), and small planets suitable for the atmospheric observations (green and pur￾ple in [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]
Figure 9
Figure 9. Figure 9: TESS light curves of TOI-654 from the PDC-SAP flux in its sectors 9, 36, 45, 46, 62, and 72 (Section 2.1). The transit windows are marked in orange ( [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]
Figure 10
Figure 10. Figure 10: The ZTF light curves in g-, r-, and i-bands, and ASAS-SN light curves in V- and g-bands (Section 3.1.3). Alt text: Time-series flux for the ZTF and ASAS-SN data [PITH_FULL_IMAGE:figures/full_fig_p013_10.png]
Figure 11
Figure 11. Figure 11: Periodograms for the TESS light curves, ZTF light curves in g-, r-, and i-bands, and ASAS-SN light curves in V- and g-bands (blue), and their window functions (gray), with the GLS for TOI-654 (Section 3.1.3). In each of the panel, the vertical line represent the orbit…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

136 extracted references · 4 linked inside Pith

  1. [1]

    2020, , 159, 123, 10.3847/1538-3881/ab4fee

    Agol , E., Luger , R., & Foreman-Mackey , D. 2020, , 159, 123, 10.3847/1538-3881/ab4fee

    doi:10.3847/1538-3881/ab4fee 2020

  2. [2]

    2014, in IAU Symposium, Vol

    Allard , F. 2014, in IAU Symposium, Vol. 299, Exploring the Formation and Evolution of Planetary Systems, ed. M. Booth , B. C. Matthews , & J. R. Graham , 271--272, 10.1017/S1743921313008545

    doi:10.1017/s1743921313008545 2014

  3. [3]

    P., Narita , N., et al

    Barkaoui , K., Schwarz , R. P., Narita , N., et al. 2024, , 687, A264, 10.1051/0004-6361/202349127

    doi:10.1051/0004-6361/202349127 2024

  4. [4]

    M., Rowe , J

    Batalha , N. M., Rowe , J. F., Bryson , S. T., et al. 2013, , 204, 24, 10.1088/0067-0049/204/2/24

    doi:10.1088/0067-0049/204/2/24 2013

  5. [5]

    C., Kulkarni , S

    Bellm , E. C., Kulkarni , S. R., Graham , M. J., et al. 2019, , 131, 018002, 10.1088/1538-3873/aaecbe

    doi:10.1088/1538-3873/aaecbe 2019

  6. [6]

    2019, , 887, L14, 10.3847/2041-8213/ab59dc

    Benneke , B., Wong , I., Piaulet , C., et al. 2019, , 887, L14, 10.3847/2041-8213/ab59dc

    doi:10.3847/2041-8213/ab59dc 2019

  7. [7]

    2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    Benneke , B., Roy , P.-A., Coulombe , L.-P., et al. 2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    arXiv doi:10.48550/arxiv.2403.03325 2024

  8. [8]

    G., et al

    Bonfanti , A., Brady , M., Wilson , T. G., et al. 2024, , 682, A66, 10.1051/0004-6361/202348180

    doi:10.1051/0004-6361/202348180 2024

Show all 136 references
  1. [9]

    J., Koch , D

    Borucki , W. J., Koch , D. G., Basri , G., et al. 2011, , 736, 19, 10.1088/0004-637X/736/1/19

    2011 doi

  2. [10]

    Brande , J., Crossfield , I. J. M., Kreidberg , L., et al. 2024, , 961, L23, 10.3847/2041-8213/ad1b5c

    2024 doi

  3. [11]

    K., et al

    Bryson , S., Kunimoto , M., Kopparapu , R. K., et al. 2021, , 161, 36, 10.3847/1538-3881/abc418

    2021 doi

  4. [12]

    2024, Nature Astronomy, 8, 463, 10.1038/s41550-023-02183-7

    Burn , R., Mordasini , C., Mishra , L., et al. 2024, Nature Astronomy, 8, 463, 10.1038/s41550-023-02183-7

    2024 doi

  5. [13]

    J., et al

    Cadieux , C., Doyon , R., MacDonald , R. J., et al. 2024, , 970, L2, 10.3847/2041-8213/ad5afa

    2024 doi

  6. [14]

    2024, , 689, A250, 10.1051/0004-6361/202450957

    Castro-Gonz \'a lez , A., Bourrier , V., Lillo-Box , J., et al. 2024, , 689, A250, 10.1051/0004-6361/202450957

    2024 doi

  7. [15]

    K., Irwin , J., et al

    Charbonneau , D., Berta , Z. K., Irwin , J., et al. 2009, , 462, 891, 10.1038/nature08679

    2009 doi

  8. [16]

    2017, , 834, 17, 10.3847/1538-4357/834/1/17

    Chen , J., & Kipping , D. 2017, , 834, 17, 10.3847/1538-4357/834/1/17

    2017 doi

  9. [17]

    2021, , 162, 174, 10.3847/1538-3881/ac1584

    Cloutier , R., Charbonneau , D., Deming , D., Bonfils , X., & Astudillo-Defru , N. 2021, , 162, 174, 10.3847/1538-3881/ac1584

    2021 doi

  10. [18]

    2020, , 159, 211, 10.3847/1538-3881/ab8237

    Cloutier , R., & Menou , K. 2020, , 159, 211, 10.3847/1538-3881/ab8237

    2020 doi

  11. [19]

    2017, , 608, A35, 10.1051/0004-6361/201731558

    Cloutier , R., Astudillo-Defru , N., Doyon , R., et al. 2017, , 608, A35, 10.1051/0004-6361/201731558

    2017 doi

  12. [20]

    E., Irwin , J., et al

    Cloutier , R., Rodriguez , J. E., Irwin , J., et al. 2020 a , , 160, 22, 10.3847/1538-3881/ab9534

    2020 doi

  13. [21]

    D., Rodriguez , J

    Cloutier , R., Eastman , J. D., Rodriguez , J. E., et al. 2020 b , , 160, 3, 10.3847/1538-3881/ab91c2

    2020 doi

  14. [22]

    M., Bonfils , X., et al

    Cointepas , M., Almenara , J. M., Bonfils , X., et al. 2021, , 650, A145, 10.1051/0004-6361/202140328

    2021 doi

  15. [23]

    2019, in American Astronomical Society Meeting Abstracts, Vol

    Collins , K. 2019, in American Astronomical Society Meeting Abstracts, Vol. 233, American Astronomical Society Meeting Abstracts \#233, 140.05

    2019

  16. [24]

    F., Almenara , J

    D \' az , R. F., Almenara , J. M., Santerne , A., et al. 2014, , 441, 983, 10.1093/mnras/stu601

    2014 doi

  17. [25]

    2022, , 164, 15, 10.3847/1538-3881/ac6bf9

    Edwards , B., & Tinetti , G. 2022, , 164, 15, 10.3847/1538-3881/ac6bf9

    2022 doi

  18. [26]

    R., Gupta , A., Sotin , C., & Valio , A

    Estrela , R., Swain , M. R., Gupta , A., Sotin , C., & Valio , A. 2020, , 898, 104, 10.3847/1538-4357/ab9a4d

    2020 doi

  19. [27]

    Ford , E. B. 2006, , 642, 505, 10.1086/500802

    2006 doi

  20. [28]

    2023, dfm/tinygp: The tiniest of Gaussian Process libraries , v0.2.4rc1, Zenodo, Zenodo, 10.5281/zenodo.7646759

    Foreman-Mackey , D. 2023, dfm/tinygp: The tiniest of Gaussian Process libraries , v0.2.4rc1, Zenodo, Zenodo, 10.5281/zenodo.7646759

    2023 doi

  21. [29]

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

    Foreman-Mackey , D., Hogg , D. W., Lang , D., & Goodman , J. 2013, , 125, 306, 10.1086/670067

    2013 doi

  22. [30]

    J., et al

    Fukui , A., Narita , N., Tristram , P. J., et al. 2011, , 63, 287, 10.1093/pasj/63.1.287

    2011 doi

  23. [31]

    2016, , 819, 27, 10.3847/0004-637X/819/1/27

    Fukui , A., Narita , N., Kawashima , Y., et al. 2016, , 819, 27, 10.3847/0004-637X/819/1/27

    2016 doi

  24. [32]

    H., et al

    Fukui , A., Korth , J., Livingston , J. H., et al. 2021, , 162, 167, 10.3847/1538-3881/ac13a5

    2021 doi

  25. [33]

    2022, , 74, L1, 10.1093/pasj/psab106

    Fukui , A., Kimura , T., Hirano , T., et al. 2022, , 74, L1, 10.1093/pasj/psab106

    2022 doi

  26. [34]

    J., Petigura , E

    Fulton , B. J., Petigura , E. A., Blunt , S., & Sinukoff , E. 2018, , 130, 044504, 10.1088/1538-3873/aaaaa8

    2018 doi

  27. [35]

    J., Petigura , E

    Fulton , B. J., Petigura , E. A., Howard , A. W., et al. 2017, , 154, 109, 10.3847/1538-3881/aa80eb

    2017 doi

  28. [36]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1, 10.1051/0004-6361/202243940

    2023 doi

  29. [37]

    L., & Rowe , J

    Gaidos , E., Ali , A., Kraus , A. L., & Rowe , J. F. 2024, , 10.1093/mnras/stae2207

    2024 doi

  30. [38]

    Gao , P., Piette , A. A. A., Steinrueck , M. E., et al. 2023, , 951, 96, 10.3847/1538-4357/acd16f

    2023 doi

  31. [39]

    P., Mather , J

    Gardner , J. P., Mather , J. C., Clampin , M., et al. 2006, , 123, 485, 10.1007/s11214-006-8315-7

    2006 doi

  32. [40]

    E., & Sari , R

    Ginzburg , S., Schlichting , H. E., & Sari , R. 2018, , 476, 759, 10.1093/mnras/sty290

    2018 doi

  33. [41]

    R., Caballero , J

    Gonz \'a lez- \'A lvarez , E., Zapatero Osorio , M. R., Caballero , J. A., et al. 2023, , 675, A177, 10.1051/0004-6361/202346292

    2023 doi

  34. [42]

    T., Irwin , M

    Gonz \'a lez-Fern \'a ndez , C., Hodgkin , S. T., Irwin , M. J., et al. 2018, , 474, 5459, 10.1093/mnras/stx3073

    2018 doi

  35. [43]

    M., Seager , S., Huang , C

    Guerrero , N. M., Seager , S., Huang , C. X., et al. 2021, , 254, 39, 10.3847/1538-4365/abefe1

    2021 doi

  36. [44]

    Gupta , A., Nicholson , L., & Schlichting , H. E. 2022, , 516, 4585, 10.1093/mnras/stac2488

    2022 doi

  37. [45]

    Gupta , A., & Schlichting , H. E. 2019, , 487, 24, 10.1093/mnras/stz1230

    2019 doi

  38. [46]

    2021, , 504, 4634, 10.1093/mnras/stab1128

    ---. 2021, , 504, 4634, 10.1093/mnras/stab1128

    2021 doi

  39. [47]

    2008, , 486, 951, 10.1051/0004-6361:200809724

    Gustafsson , B., Edvardsson , B., Eriksson , K., et al. 2008, , 486, 951, 10.1051/0004-6361:200809724

    2008 doi

  40. [48]

    T., Fabrycky , D

    Hamann , A., Montet , B. T., Fabrycky , D. C., Agol , E., & Kruse , E. 2019, , 158, 133, 10.3847/1538-3881/ab32e3

    2019 doi

  41. [49]

    2022, , 74, 904, 10.1093/pasj/psac044

    Harakawa , H., Takarada , T., Kasagi , Y., et al. 2022, , 74, 904, 10.1093/pasj/psac044

    2022 doi

  42. [50]

    J., Hey , D., et al

    Hart , K., Shappee , B. J., Hey , D., et al. 2023, arXiv e-prints, arXiv:2304.03791, 10.48550/arXiv.2304.03791

    2023 doi arXiv

  43. [51]

    2024, exoplanet-dev/jaxoplanet: Astronomical time series analysis with JAX , v0.0.2, Zenodo, 10.5281/zenodo.10736936

    Hattori, S., Garcia, L., Murray, C., et al. 2024, exoplanet-dev/jaxoplanet: Astronomical time series analysis with JAX , v0.0.2, Zenodo, 10.5281/zenodo.10736936

    2024 doi

  44. [52]

    2024, , 76, 1131, 10.1093/pasj/psae075

    Hayashi , Y., Narita , N., Fukui , A., et al. 2024, , 76, 1131, 10.1093/pasj/psae075

    2024 doi

  45. [53]

    2018, , 155, 127, 10.3847/1538-3881/aaa9c1

    Hirano , T., Dai , F., Gandolfi , D., et al. 2018, , 155, 127, 10.3847/1538-3881/aaa9c1

    2018 doi

  46. [54]

    2020 a , , 899, L13, 10.3847/2041-8213/aba6eb

    Hirano , T., Krishnamurthy , V., Gaidos , E., et al. 2020 a , , 899, L13, 10.3847/2041-8213/aba6eb

    2020 doi

  47. [55]

    2020 b , , 72, 93, 10.1093/pasj/psaa085

    Hirano , T., Kuzuhara , M., Kotani , T., et al. 2020 b , , 72, 93, 10.1093/pasj/psaa085

    2020 doi

  48. [56]

    H., Fukui , A., et al

    Hirano , T., Livingston , J. H., Fukui , A., et al. 2021, , 162, 161, 10.3847/1538-3881/ac0fdc

    2021 doi

  49. [57]

    H., et al

    Hirano , T., Dai , F., Livingston , J. H., et al. 2023, , 165, 131, 10.3847/1538-3881/acb7e1

    2023 doi

  50. [58]

    2024, , 530, 3117, 10.1093/mnras/stae998

    Hirano , T., Gaidos , E., Harakawa , H., et al. 2024, , 530, 3117, 10.1093/mnras/stae998

    2024 doi

  51. [59]

    Ho , C. S. K., Rogers , J. G., Van Eylen , V., Owen , J. E., & Schlichting , H. E. 2024, , 531, 3698, 10.1093/mnras/stae1376

    2024 doi

  52. [60]

    Ho , C. S. K., & Van Eylen , V. 2023, , 519, 4056, 10.1093/mnras/stac3802

    2023 doi

  53. [61]

    D., Gelman, A., et al

    Hoffman, M. D., Gelman, A., et al. 2014, J. Mach. Learn. Res., 15, 1593

    2014

  54. [62]

    J., Kempton , E

    Hord , B. J., Kempton , E. M. R., Evans-Soma , T. M., et al. 2024, , 167, 233, 10.3847/1538-3881/ad3068

    2024 doi

  55. [63]

    2024, , 167, 289, 10.3847/1538-3881/ad4115

    Hori , Y., Fukui , A., Hirano , T., et al. 2024, , 167, 289, 10.3847/1538-3881/ad4115

    2024 doi

  56. [64]

    O., Wende-von Berg , S., Dreizler , S., et al

    Husser , T. O., Wende-von Berg , S., Dreizler , S., et al. 2013, , 553, A6, 10.1051/0004-6361/201219058

    2013 doi

  57. [65]

    2012, , 753, 66, 10.1088/0004-637X/753/1/66

    Ikoma , M., & Hori , Y. 2012, , 753, 66, 10.1088/0004-637X/753/1/66

    2012 doi

  58. [66]

    2020, , 902, 73, 10.3847/1538-4357/abae5f

    Ikuta , K., Maehara , H., Notsu , Y., et al. 2020, , 902, 73, 10.3847/1538-4357/abae5f

    2020 doi

  59. [67]

    K., & Schlichting , H

    Inamdar , N. K., & Schlichting , H. E. 2015, , 448, 1751, 10.1093/mnras/stv030

    2015 doi

  60. [68]

    T., Aoki , W., Kotani , T., et al

    Ishikawa , H. T., Aoki , W., Kotani , T., et al. 2020, , 72, 102, 10.1093/pasj/psaa101

    2020 doi

  61. [69]

    T., Aoki , W., Hirano , T., et al

    Ishikawa , H. T., Aoki , W., Hirano , T., et al. 2022, , 163, 72, 10.3847/1538-3881/ac3ee0

    2022 doi

  62. [70]

    M., Twicken , J

    Jenkins , J. M., Twicken , J. D., McCauliff , S., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9913, Software and Cyberinfrastructure for Astronomy IV, ed. G. Chiozzi & J. C. Guzman , 99133E, 10.1117/12.2233418

    2016 doi

  63. [71]

    2023, , 75, 713, 10.1093/pasj/psad031

    Kagetani , T., Narita , N., Kimura , T., et al. 2023, , 75, 713, 10.1093/pasj/psad031

    2023 doi

  64. [72]

    E., & Raftery, A

    Kass, R. E., & Raftery, A. E. 1995, Journal of the American Statistical Association, 90, 773, 10.1080/01621459.1995.10476572

    1995

  65. [73]

    2022, , 666, A4, 10.1051/0004-6361/202243381

    Kawauchi , K., Murgas , F., Palle , E., et al. 2022, , 666, A4, 10.1051/0004-6361/202243381

    2022 doi

  66. [74]

    Kempton , E. M. R., Bean , J. L., Louie , D. R., et al. 2018, , 130, 114401, 10.1088/1538-3873/aadf6f

    2018 doi

  67. [75]

    Kempton , E. M. R., Zhang , M., Bean , J. L., et al. 2023, , 620, 67, 10.1038/s41586-023-06159-5

    2023 doi

  68. [76]

    2022, Nature Astronomy, 6, 1296, 10.1038/s41550-022-01781-1

    Kimura , T., & Ikoma , M. 2022, Nature Astronomy, 6, 1296, 10.1038/s41550-022-01781-1

    2022 doi

  69. [77]

    Kipping , D. M. 2013, , 435, 2152, 10.1093/mnras/stt1435

    2013 doi

  70. [78]

    S., Shappee , B

    Kochanek , C. S., Shappee , B. J., Stanek , K. Z., et al. 2017, , 129, 104502, 10.1088/1538-3873/aa80d9

    2017 doi

  71. [79]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Kotani , T., Tamura , M., Nishikawa , J., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Ground-based and Airborne Instrumentation for Astronomy VII, ed. C. J. Evans , L. Simard , & H. Takami , 1070211, 10.1117/12.2311836

    2018 doi

  72. [80]

    2023, , 521, 1210, 10.1093/mnras/stad404

    Krishnamurthy , V., Hirano , T., Gaidos , E., et al. 2023, , 521, 1210, 10.1093/mnras/stad404

    2023 doi

  73. [81]

    A., Stempels , H

    Kupka , F., Piskunov , N., Ryabchikova , T. A., Stempels , H. C., & Weiss , W. W. 1999, , 138, 119, 10.1051/aas:1999267

    1999 doi

  74. [82]

    2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Kuzuhara , M., Hirano , T., Kotani , T., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10702, Ground-based and Airborne Instrumentation for Astronomy VII, ed. C. J. Evans , L. Simard , & H. Takami , 1070260, 10.1117/12.2311832

    2018 doi

  75. [83]

    H., et al

    Kuzuhara , M., Fukui , A., Livingston , J. H., et al. 2024, , 967, L21, 10.3847/2041-8213/ad3642

    2024 doi

  76. [84]

    2024, , 692, A238, 10.1051/0004-6361/202452244

    Lacedelli , G., Pall \'e , E., Luque , R., et al. 2024, , 692, A238, 10.1051/0004-6361/202452244

    2024 doi

  77. [85]

    Lam , K. W. F., Korth , J., Masuda , K., et al. 2020, , 159, 120, 10.3847/1538-3881/ab66c9

    2020 doi

  78. [86]

    J., Chiang , E., & Ormel , C

    Lee , E. J., Chiang , E., & Ormel , C. W. 2014, , 797, 95, 10.1088/0004-637X/797/2/95

    2014 doi

  79. [87]

    Liu , S.-F., Hori , Y., Lin , D. N. C., & Asphaug , E. 2015, , 812, 164, 10.1088/0004-637X/812/2/164

    2015 doi

  80. [88]

    Lopez , E. D. 2017, , 472, 245, 10.1093/mnras/stx1558

    2017 doi

  81. [89]

    D., & Fortney , J

    Lopez , E. D., & Fortney , J. J. 2013, , 776, 2, 10.1088/0004-637X/776/1/2

    2013 doi

  82. [90]

    D., & Rice , K

    Lopez , E. D., & Rice , K. 2018, , 479, 5303, 10.1093/mnras/sty1707

    2018 doi

  83. [91]

    2022, Science, 377, 1211, 10.1126/science.abl7164

    Luque , R., & Pall \'e , E. 2022, Science, 377, 1211, 10.1126/science.abl7164

    2022 doi

  84. [92]

    S., Eastman , J

    Mahajan , A. S., Eastman , J. D., & Kirk , J. 2024, , 963, L37, 10.3847/2041-8213/ad29f3

    2024 doi

  85. [93]

    W., Feiden , G

    Mann , A. W., Feiden , G. A., Gaidos , E., Boyajian , T., & von Braun , K. 2015, , 804, 64, 10.1088/0004-637X/804/1/64

    2015 doi

  86. [94]

    W., Dupuy , T., Kraus , A

    Mann , A. W., Dupuy , T., Kraus , A. L., et al. 2019, , 871, 63, 10.3847/1538-4357/aaf3bc

    2019 doi

  87. [95]

    J., Laher , R

    Masci , F. J., Laher , R. R., Rusholme , B., et al. 2019, , 131, 018003, 10.1088/1538-3873/aae8ac

    2019 doi

  88. [96]

    2016, , 589, A75, 10.1051/0004-6361/201528065

    Mazeh , T., Holczer , T., & Faigler , S. 2016, , 589, A75, 10.1051/0004-6361/201528065

    2016 doi

  89. [97]

    H., Harbeck , D.-R., et al

    McCully , C., Volgenau , N. H., Harbeck , D.-R., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10707, Software and Cyberinfrastructure for Astronomy V, ed. J. C. Guzman & J. Ibsen , 107070K, 10.1117/12.2314340

    2018 doi

  90. [98]

    H., Leon , J

    Mori , M., Livingston , J. H., Leon , J. d., et al. 2022, , 163, 298, 10.3847/1538-3881/ac6bf8

    2022 doi

  91. [99]

    2021, , 653, A60, 10.1051/0004-6361/202140718

    Murgas , F., Astudillo-Defru , N., Bonfils , X., et al. 2021, , 653, A60, 10.1051/0004-6361/202140718

    2021 doi

  92. [100]

    2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 045001, 10.1117/1.JATIS.1.4.045001

    Narita , N., Fukui , A., Kusakabe , N., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 045001, 10.1117/1.JATIS.1.4.045001

    2015 doi

  93. [101]

    2019, Journal of Astronomical Telescopes, Instruments, and Systems, 5, 015001, 10.1117/1.JATIS.5.1.015001

    ---. 2019, Journal of Astronomical Telescopes, Instruments, and Systems, 5, 015001, 10.1117/1.JATIS.5.1.015001

    2019 doi

  94. [102]

    2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Narita , N., Fukui , A., Yamamuro , T., et al. 2020, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 11447, Ground-based and Airborne Instrumentation for Astronomy VIII, ed. C. J. Evans , J. J. Bryant , & K. Motohara , 114475K, 10.1117/12.2559947

    2020 doi

  95. [103]

    E., Ford , E

    Nelson , B. E., Ford , E. B., Buchner , J., et al. 2020, , 159, 73, 10.3847/1538-3881/ab5190

    2020 doi

  96. [104]

    2020, , 642, A173, 10.1051/0004-6361/202037867

    Nowak , G., Luque , R., Parviainen , H., et al. 2020, , 642, A173, 10.1051/0004-6361/202037867

    2020 doi

  97. [105]

    E., & Schlichting , H

    Owen , J. E., & Schlichting , H. E. 2024, , 528, 1615, 10.1093/mnras/stad3972

    2024 doi

  98. [106]

    E., & Wu , Y

    Owen , J. E., & Wu , Y. 2013, , 775, 105, 10.1088/0004-637X/775/2/105

    2013 doi

  99. [107]

    2017, , 847, 29, 10.3847/1538-4357/aa890a

    ---. 2017, , 847, 29, 10.3847/1538-4357/aa890a

    2017 doi

  100. [108]

    2024, , 688, A59, 10.1051/0004-6361/202449911

    Parc , L., Bouchy , F., Venturini , J., Dorn , C., & Helled , R. 2024, , 688, A59, 10.1051/0004-6361/202449911

    2024 doi

  101. [109]

    2015, , 453, 3821, 10.1093/mnras/stv1857

    Parviainen , H., & Aigrain , S. 2015, , 453, 3821, 10.1093/mnras/stv1857

    2015 doi

  102. [110]

    2024, , 683, A170, 10.1051/0004-6361/202347431

    Parviainen , H., Murgas , F., Esparza-Borges , E., et al. 2024, , 683, A170, 10.1051/0004-6361/202347431

    2024 doi

  103. [111]

    J., & Mamajek , E

    Pecaut , M. J., & Mamajek , E. E. 2013, , 208, 9, 10.1088/0067-0049/208/1/9

    2013 doi

  104. [112]

    2024, , 690, A62, 10.1051/0004-6361/202347251

    Pel \'a ez-Torres , A., Esparza-Borges , E., Pall \'e , E., et al. 2024, , 690, A62, 10.1051/0004-6361/202347251

    2024 doi

  105. [113]

    A., Rogers , J

    Petigura , E. A., Rogers , J. G., Isaacson , H., et al. 2022, , 163, 179, 10.3847/1538-3881/ac51e3

    2022 doi

  106. [114]

    2019, arXiv preprint arXiv:1912.11554

    Phan, D., Pradhan, N., & Jankowiak, M. 2019, arXiv preprint arXiv:1912.11554

    2019 arXiv

  107. [115]

    R., Winn , J

    Ricker , G. R., Winn , J. N., Vanderspek , R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003, 10.1117/1.JATIS.1.1.014003

    2015 doi

  108. [116]

    G., Gupta , A., Owen , J

    Rogers , J. G., Gupta , A., Owen , J. E., & Schlichting , H. E. 2021, , 508, 5886, 10.1093/mnras/stab2897

    2021 doi

  109. [117]

    G., Owen , J

    Rogers , J. G., Owen , J. E., & Schlichting , H. E. 2024, , 529, 2716, 10.1093/mnras/stae563

    2024 doi

  110. [118]

    G., Schlichting , H

    Rogers , J. G., Schlichting , H. E., & Owen , J. E. 2023, , 947, L19, 10.3847/2041-8213/acc86f

    2023 doi

  111. [119]

    L., et al

    Ryabchikova , T., Piskunov , N., Kurucz , R. L., et al. 2015, , 90, 054005, 10.1088/0031-8949/90/5/054005

    2015 doi

  112. [120]

    F., Almenara , J

    Santerne , A., D \' az , R. F., Almenara , J. M., et al. 2015, , 451, 2337, 10.1093/mnras/stv1080

    2015 doi

  113. [121]

    2018, , 155, 257, 10.3847/1538-3881/aac108

    Sarkis , P., Henning , T., K \"u rster , M., et al. 2018, , 155, 257, 10.3847/1538-3881/aac108

    2018 doi

  114. [122]

    2011, , 417, 2166, 10.1111/j.1365-2966.2011.19399.x

    Southworth , J. 2011, , 417, 2166, 10.1111/j.1365-2966.2011.19399.x

    2011

  115. [123]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, , 158, 138, 10.3847/1538-3881/ab3467

    2019 doi

  116. [124]

    M., & Kiss , L

    Szab \'o , G. M., & Kiss , L. L. 2011, , 727, L44, 10.1088/2041-8205/727/2/L44

    2011 doi

  117. [125]

    2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tamura , N., Takato , N., Iwamuro , F., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV, ed. I. S. McLean , S. K. Ramsay , & H. Takami , 84460M, 10.1117/12.925831

    2012 doi

  118. [126]

    2018, Experimental Astronomy, 46, 135, 10.1007/s10686-018-9598-x

    Tinetti , G., Drossart , P., Eccleston , P., et al. 2018, Experimental Astronomy, 46, 135, 10.1007/s10686-018-9598-x

    2018 doi

  119. [127]

    1978, , 62, 29

    Tsuji , T. 1978, , 62, 29

    1978

  120. [128]

    S., et al

    Van Eylen , V., Agentoft , C., Lundkvist , M. S., et al. 2018, , 479, 4786, 10.1093/mnras/sty1783

    2018 doi

  121. [129]

    2021, , 507, 2154, 10.1093/mnras/stab2143

    Van Eylen , V., Astudillo-Defru , N., Bonfils , X., et al. 2021, , 507, 2154, 10.1093/mnras/stab2143

    2021 doi

  122. [130]

    M., Haldemann , J., Ronco , M

    Venturini , J., Guilera , O. M., Haldemann , J., Ronco , M. P., & Mordasini , C. 2020, , 643, L1, 10.1051/0004-6361/202039141

    2020 doi

  123. [131]

    P., Guilera , O

    Venturini , J., Ronco , M. P., Guilera , O. M., et al. 2024, , 686, L9, 10.1051/0004-6361/202349088

    2024 doi

  124. [132]

    Winn , J. N. 2010, in Exoplanets, ed. S. Seager , 55--77, 10.48550/arXiv.1001.2010

    2010 doi arXiv

  125. [133]

    2009, , 496, 577, 10.1051/0004-6361:200811296

    Zechmeister , M., & K \"u rster , M. 2009, , 496, 577, 10.1051/0004-6361:200811296

    2009 doi

  126. [134]

    J., et al

    Zechmeister , M., Reiners , A., Amado , P. J., et al. 2018, , 609, A12, 10.1051/0004-6361/201731483

    2018 doi

  127. [135]

    B., Sasselov , D

    Zeng , L., Jacobsen , S. B., Sasselov , D. D., et al. 2019, Proceedings of the National Academy of Science, 116, 9723, 10.1073/pnas.1812905116

    2019 doi

  128. [136]

    \@bibitem \@bib@author\@prev@author \@set@biblabel \@lbibitem[#1] \@bib@parse#1()\@nil \@set@biblabel \@bib@parse#1(#2)#3\@nil \@bib@author #1 @edef\@bib@year @space#2 \@empty \@set@biblabel#1 \@bib@author\@empty \@latex@warning Author name should be given for reference entry ...

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.