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REVIEW 3 major objections 6 minor 127 references

Discovery of a transiting hot water-world candidate orbiting Ross 176 with TESS and CARMENES

T0 review · 3 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read TESS and CARMENES confirm a transiting hot planet around Ross 176, and its density points to a water-rich composition.

desk verdict Secure discovery of a small transiting planet around a K7V star, but the mass and especially the eccentricity rest on a GP+Keplerian fit with incomplete phase coverage, and the water-world label is a stretch. read the letter →

arxiv 2507.15763 v1 pith:X5LYSUTT submitted 2025-07-21 astro-ph.EP

S. Geraldía-González , J. Orell-Miquel , E. Pallé , F. Murgas , G. Lacedelli , V. J. S. Béjar , J. A. Caballero , C. Duque-Arribas
show 25 more authors
J. Lillo-Box D. Montes G. Morello E. Nagel A. Schweitzer H. M. Tabernero Y. Calatayud-Borras C. Cifuentes G. Fernández-Rodríguez A. Fukui J. de Leon N. Lodieu R. Luque M. Mori N. Narita H. Parviainen E. Poultourtzidis A. Reiners I. Ribas M. Schlecker S. Seager K. G. Stassun T. Trifonov S. Vanaverbeke J. N. Winn
This is my paper · ORCID
classification astro-ph.EP
keywords Ross176TOI-4491waterworldK-typestartransitingexoplanetradialvelocitiesTESSradiusvalley
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 reports the confirmation and characterization of a transiting planet around the late K-type star Ross 176, and argues that the planet's bulk properties are consistent with a water-world composition. The evidence combines five sectors of TESS photometry, two ground-based multiband transits, and 99 CARMENES radial-velocity measurements, with Gaussian-process models used to subtract the host star's activity. If the result holds, Ross 176 b becomes one of the few small planets around a K dwarf with mass measured to better than 20%, sitting inside the radius valley and offering a concrete target for JWST to test whether such worlds are water-rich or gas-dominated.

What carries the argument

The central machinery is a joint fit of the TESS and MuSCAT2 light curves together with the CARMENES radial velocities, in which stellar activity is modeled with a quasi-periodic Gaussian-process kernel whose rotation-period hyperparameter is centered near 16 days, the first harmonic of the roughly 32-day stellar rotation. This Gaussian process is what lets the small Keplerian semi-amplitude $K = 2.55$ m/s be attributed to the planet rather than to spots or rotation. A second piece of machinery, the ExoMDN machine-learning interior retrieval, converts mass, radius, and equilibrium temperature into core, mantle, water, and gas fractions under a layered-structure assumption.

What would settle it

Measure Ross 176's radial velocities from a second longitude over additional seasons and re-fit without fixing the Gaussian-process period: if the 32-day or 16-day activity signals reappear in the residuals, or if the recovered semi-amplitude and eccentricity move by more than the quoted uncertainties, the mass and eccentricity claims fail. Separately, a JWST transmission spectrum that detects strong H/He features would rule out the bare water-world scenario, while a featureless spectrum at the simulated precision would support it.

Watch

Extended reading notes

Core claim

On the paper's own terms, Ross 176 b is a genuine transiting hot planet with orbital period $P = 5.0066338$ days, radius $R_p = 1.84 \pm 0.08\,R_\oplus$, mass $M_p = 4.57^{+0.89}_{-0.93}\,M_\oplus$, mean density $\rho_p = 4.03^{+0.49}_{-0.81}$ g cm$^{-3}$, and eccentricity $e = 0.25 \pm 0.04$. The radius detection is quoted at about $23\sigma$ and the mass at about $5\sigma$. With an equilibrium temperature near 682 K the planet is too hot for surface habitability, and its position in the mass-radius diagram, inside the radius gap and near Wolf 503 b, makes it a water-world candidate: the ExoMDN interior retrieval gives a 14% water mass fraction whose upper uncertainty overlaps a 50% water composition. The paper also simulates JWST transmission spectra and finds that one transit could reveal an H/He atmosphere if present, while a flat spectrum would favor the water-world interpretation.

Load-bearing premise

The mass and eccentricity rest on the assumption that the Gaussian-process activity model fully removes the star's rotation-related noise from the radial velocities, even though a single site did not cover all orbital phases; the water-world reading further assumes a layered internal structure.

Editorial extensions

If this is right

  • Ross 176 b joins the small sample of planets around K-type stars with both radius and mass measured to high precision, making it a test case for whether the radius valley exists for K dwarfs and what sculpts it.
  • If the water-world reading is correct, the planet offers a close K-star analog to Wolf 503 b and HD 40307 b, allowing comparisons of water-world formation and evolution under different stellar environments.
  • A single JWST transit observation could detect H/He absorption features tens to hundreds of ppm in size; a flat transmission spectrum would instead rule out a clear mini-Neptune and leave the steam or water-world scenario.
  • The refined ephemeris from the combined TESS and MuSCAT2 fit makes future transit and atmospheric observations schedulable with small timing uncertainty.
  • Because the planet is alone in the system at current detection limits, its moderate eccentricity cannot be blamed on an observed companion, which constrains dynamical explanations.

Reading between the lines

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

  • This reading treats the quoted mass and eccentricity as conditional on the 16-day Gaussian-process prior; because only part of the orbit was sampled from one site in one season, a second-longitude campaign is the direct way to check whether $K$ and $e$ shift.
  • The water-world classification inherits the layered-interior assumption of ExoMDN; comparing against non-layered or mixed-interior models would show how much of the water fraction is an artifact of that assumption.
  • If the eccentricity survives better phase coverage, tidal circularization arguments for a 5-day planet around a K dwarf become harder to satisfy, which would point to a recent dynamical perturbation or an unseen longer-period companion.
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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

3 major / 6 minor

Summary. The paper reports the discovery and characterization of a transiting small planet, Ross 176 b, around a late K-type star using TESS photometry, two ground-based MuSCAT2 transits, and 99 CARMENES radial velocities. The authors derive an orbital period of about 5.0066 d, a planetary radius of Rp = 1.84 ± 0.08 R⊕, a mass of Mp = 4.57 +0.89/−0.93 M⊕, a mean density of 4.03 g cm−3, and an eccentricity of e = 0.25 ± 0.04. They model stellar activity with Gaussian processes, compare Bayesian evidences for competing RV models, and use the ExoMDN machine-learning tool to infer an interior composition that they interpret as consistent with a water-world candidate. They also present synthetic JWST transmission spectra to assess the planet's suitability for atmospheric follow-up. The central detection is supported by three independent data sets, while the mass, eccentricity, and composition claims rely on the joint GP+Keplerian modeling and are acknowledged by the authors to be limited by single-season phase coverage and by the layered-structure assumption of the interior model.

Significance. If the derived parameters hold, Ross 176 b adds a well-characterized small planet (radius precision 4%, mass precision 20%) to the sparse sample of small planets around K-type stars, and it lies inside the radius valley, making it relevant for formation and evolution studies. The paper is also valuable as a demonstration of combining TESS, ground-based photometry, and CARMENES RVs with GP activity modeling. The JWST forward-modeling section provides useful, concrete predictions for future observations. The authors are appropriately cautious in the discussion of the interior composition and acknowledge the principal caveats; however, the title and abstract present the water-world interpretation more strongly than the data justify.

major comments (3)
  1. [Sect. 5.2, Table A.1, Fig. A.5] The 5σ significance quoted for K (and hence Mp) is based on the posterior of K, but the RV detection is strongly model-dependent: the Keplerian-only model is disfavoured relative to a flat line (logZ = −293.34 vs −290.40), and the signal only emerges once a quasi-periodic GP is included. Because the GP amplitude (23 ± 7 m/s) is nearly ten times larger than K and the GP coherence length is L = 40 d, the GP can in principle absorb part of the 5-d signal. The paper does not provide an injection-recovery test or a GP-only model with the same N(16,2) hyperprior used in the preferred planet+GP model. I request a sensitivity analysis of the K posterior to the GPProt and L priors, along with a recovery test of injected Keplerian signals, to demonstrate that K is not biased by the activity model.
  2. [Sect. 5.3, Sect. 6.4, Table 2] The eccentricity e = 0.25 ± 0.04 and ω are derived from 99 RVs from a single site and season, and Sect. 6.4 acknowledges that the 5-d period prevents full orbital-phase coverage. With K ≈ 2.55 m/s, e and ω are strongly degenerate with K, and the reported eccentricity posterior may be driven by the prior bound e < 0.5 and by the incomplete phase sampling rather than by a robust detection of non-circularity. The paper should show the RV phase coverage, report the joint fit with a circular orbit, and quantify how much of the ΔlogZ ≈ 9.3 preference for the eccentric model comes from the GP activity component. Without this, the quoted density and the subsequent water-world classification rest on a fragile eccentric solution.
  3. [Sect. 6.2, Abstract, Title] The ExoMDN water mass fraction is wWater = 0.14 +0.24/−0.13, which is consistent with zero at about 1σ and with the 50% water-world value at only about 1.5σ. The text itself acknowledges that the lower uncertainty is consistent with no water and that the layered-structure assumption 'may not be the case for water worlds and sub-Neptunes in general.' Given this, calling Ross 176 b a 'hot water-world candidate' in the title and abstract overstates the evidence. I recommend softening the classification to 'water-world candidate' with a clear quantitative caveat in the abstract, or adding a dedicated model-comparison analysis (rocky vs water-rich interiors) to justify the label.
minor comments (6)
  1. [Section 7 / Data availability] There is a typo in the heading: 'Data aviability' should be 'Data availability'.
  2. [Abstract / Sect. 6] The density unit appears as 'g m−3' in the abstract and in Sect. 6; it should be 'g cm−3' as in Table 2.
  3. [Abstract] The phrase 'is efficient for confirm new planets' is ungrammatical; it should be 'is efficient for confirming new planets'.
  4. [Abstract / Sect. 5.3] The paper describes e = 0.25 as a 'low-eccentricity orbit'; an eccentricity of 0.25 is moderate rather than low, and the wording should be adjusted for consistency with the period–eccentricity discussion in Sect. 6.4.
  5. [Sect. 5.2] The text refers to the '16-day signal' as 'the first harmonic' of the 32-day rotation, but then adopts GPProt = 17 ± 1 d. Clarify whether the GP period is intended to model the harmonic itself and how the 32-d modulation is accounted for in the RV model.
  6. [Sect. 6.4] The sentence 'The period of Ross 176 b's prevent us from covering the full orbital phases...' contains a grammatical error; it should be 'The period of Ross 176 b prevents us from covering...'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the planet parameters are derived from independent TESS photometry, MuSCAT2 transits, and CARMENES radial velocities, while the water-world classification is an explicitly hedged comparison with an externally trained interior model.

full rationale

The paper's derivation chain is self-contained. The transit detection and radius come from TESS PDC-SAP photometry plus two MuSCAT2 transits ('The two MuSCAT2 transits are included in our analysis in Sect. 5'; 'the fitting models reveal a very clear transit in joint light-curve data'), which are independent of the RV fit. The RV mass is not an input renamed as a prediction: the planetary signal is first identified in the CARMENES periodogram ('The strongest signal lies at the period of the planet detected in the photometric data with a FAP of ~1%'), and the Bayesian model comparison in Table A.1 shows the planet+GP(16 d) model (logZ = -280.80) is strongly favored over a flat line (-290.40) and over a planet-only Keplerian (-293.34), so the mass and eccentricity are genuinely constrained by the data rather than forced by the GP. The GP is used to model stellar activity, not to inject the planet. The eccentricity is fitted with free parameters and is consistent when photometry and RVs are fit jointly; the paper's own caveat about single-site phase coverage ('Further RV observations from a different location will help us to sample the missing phases and fully constrain the eccentricity') is a precision limitation, not a circular step. The water-world interpretation is an inversion of the externally trained ExoMDN model ('trained with more than six millions synthetic planet models computed from the code TATOOINE') on observed M, R, and Teq; the resulting wWater = 0.14+0.24/-0.13 is compared, not equated, with the Luque & Pallé (2022) water-world classification, and the paper explicitly notes the classification's applicability to FGK stars is uncertain and that the ExoMDN layered-structure assumption may fail. The Luque & Pallé citation is a self-citation (Pallé and Luque are co-authors), but it is used only as an interpretive benchmark and is externally falsifiable, so it does not make the argument circular. No fitted parameter is renamed as a prediction, no uniqueness theorem is invoked, and no known result is repackaged.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The detection and characterization rely on standard Bayesian transit and RV fitting with public tools, empirical stellar relations, and the layered-interior assumption in ExoMDN for the composition inference. No new physical entities are introduced. The hand-chosen inputs are the GP period prior for the activity model, the eccentricity prior bound, and the photometric GP priors; the model-comparison tables in the appendix show the central detection is not sensitive to these choices.

free parameters (3)
  • GPProt, period of the quasi-periodic GP for RV activity = Posterior 17 ± 1 d; prior N(16, 2) d
    The RV activity component uses a celerite quasi-periodic kernel with the period hyperparameter given a normal prior centered at 16 d, selected after comparing models with Prot at 8, 16, and 32 d (Table A.1). This hand-chosen prior shapes the activity correction applied before the 5 d Keplerian is measured; the frequency separation limits the impact on K.
  • Eccentricity prior bound = e drawn from a beta prior on [0, 0.5]
    The joint fit restricts eccentricity to e < 0.5. The posterior peaks at e = 0.25, away from the boundary, but the prior width still shapes the quoted 68% interval and the ΔlogZ = 9.3 preference over the circular model.
  • Light-curve GP amplitude and length scale = σ_TESS = 0.47 +3.16/-0.43 ppm; ρ_TESS ≈ 1 d; similar per MuSCAT2 band
    The photometric GP priors were 'carefully chosen to prevent fitting the transit' (Table A.2). These are standard detrending choices for correlated noise; the posterior GP amplitude is small, so the central transit parameters are not strongly affected.
assumptions (5)
  • domain assumption The Schweitzer et al. (2019) linear stellar mass-radius relation gives M* = 0.577 ± 0.024 M⊙ for Ross 176.
    Section 4.1: 'the stellar mass from the linear mass-radius relation given by Schweitzer et al. (2019)'. M* enters the conversion from the fitted RV semi-amplitude K to Mp; the quoted 4% stellar-mass precision propagates into the planet mass.
  • domain assumption The celerite quasi-periodic GP with Prot ~16 d fully captures the stellar activity contribution to the RVs.
    Section 5.2: the preferred RV model is a Keplerian plus a GP with a normal prior on Prot at 16 d. If residual activity leaks into K the mass would be biased; the ΔlogZ comparison and the clean residual periodogram support the assumption.
  • domain assumption ExoMDN/TATOOINE layered interior models (iron core, silicate mantle, water/ice layer, H/He atmosphere) describe the planet's possible internal structure.
    Section 6.2: 'ExoMDN assumes a layered internal structure, which may not be the case for water worlds and sub-Neptunes in general'. The water-fraction estimate, and hence the water-world framing, depends on this assumption.
  • domain assumption The TESS aperture dilution factor is exactly unity.
    Section 2 and Table A.2: dilution is fixed to 1 because no comparably bright star lies in the TESS aperture and PDC-SAP corrects for dilution. If an unresolved blend contributed, Rp would be overestimated.
  • standard math Nested sampling log-evidence differences select between models (Trotta 2008 thresholds).
    Used throughout Section 5 to prefer the eccentric over the circular model (ΔlogZ ≈ 9.3) and planet-plus-GP over activity-only models (Table A.1).

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Cite this review

Pith. "Pith review of Discovery of a transiting hot water-world candidate orbiting Ross 176 with TESS and CARMENES." pith.science (2026). https://pith.science/paper/X5LYSUTT

@misc{pith2026250715763,
  author       = {Pith},
  title        = {Pith review of: Discovery of a transiting hot water-world candidate orbiting Ross 176 with TESS and CARMENES},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/X5LYSUTT}},
  note         = {Machine review of arXiv:2507.15763}
}
abstract

The case of Ross 176 is a late K-type star that hosts a promising water-world candidate planet. The star has a radius of $R_*$=0.569$\pm$0.020$R_{\odot}$ and a mass of $M_{\star}$ = 0.577 $\pm$ 0.024 $M_{\odot}$. We constrained the planetary mass using spectroscopic data from CARMENES, an instrument that has already played a major role in confirming the planetary nature of the transit signal detected by TESS. We used Gaussian Processes (GP) to improve the analysis because the host star has a relatively strong activity that affects the radial velocity dataset. In addition, we applied a GP to the TESS light curves to reduce the correlated noise in the detrended dataset. The stellar activity indicators show a strong signal that is related to the stellar rotation period of $\sim$ 32 days. This stellar activity signal was also confirmed on the TESS light curves. Ross 176b is an inner hot transiting planet with a low-eccentricity orbit of $e = 0.25 \pm 0.04$, an orbital period of $P \sim 5$ days, and an equilibrium temperature of $T_{eq}\sim 682K$. With a radius of $R_p = 1.84\pm0.08R_{\oplus}$ (4% precision), a mass of $M_p = 4.57^{+0.89}_{-0.93} M_{\oplus}$ (20% precision), and a mean density of $\rho_p = 4.03^{+0.49}_{-0.81} g cm^{-3}$, the composition of Ross 176b might be consistent with a water-world scenario. Moreover, Ross 176b is a promising target for atmospheric characterization, which might lead to more information on the existence, formation and composition of water worlds. This detection increases the sample of planets orbiting K-type stars. This sample is valuable for investigating the valley of planets with small radii around this type of star. This study also shows that the dual detection of space- and ground-based telescopes is efficient for confirm new planets.

Figures

Figures reproduced from arXiv: 2507.15763 by the authors.

Figure 1
Figure 1. GLS periodogram of serval activity indicators. From top to bottom: Hα λ6562.81 Å, Na i D1 and D2 λλ 5889.9, 5895.92 Å, Ca ii IRT λλλ 8498.02, 8542.09, 8662.14 Å, CRX, and dLW periodograms. In all panels, the period of the planet candidate at 5.01 d is marked with a vertical dashed green line, and the star-related signals at 8, 16, and 32 days are marked in orange, red, and magenta, respectively. The 10%, 1%, and 0.1… view at source ↗
Figure 2
Figure 2. Periodograms with solid vertical lines that indicate the period of the planet candidate at 5 days in green and the star-related peri￾odicities at about 8, 16, and 32 days in orange, red, and magenta, re￾spectively. The 10%, 1%, and 0.1% FAP levels are marked as horizon￾tal dashed, dash-dotted, and dotted gray lines, respectively. The peaks near one day correspond to aliases of the stellar rotation signal, intro￾duce… view at source ↗
Figure 3
Figure 3. CARMENES radial velocity time series. Top panel: CARMENES data points (blue dots with error bars) along with the best-fit model. The full model is plotted in black, and the Keplerian component is shown in green and the GP model in red. Bottom panel: Residuals from the fitted model. 5.3. Joint fit In order to better constrain the planet parameters, we jointly fit the photometric and RV time series. In previous sectio… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Phase-folded joint fit of Ross 176 b. Left panel: Phase-folded transits from TESS (blue points) with the joint-fit model (black line). Right panel: Phase-folded RV data from CARMENES (red points), with the joint-fit model (black line), and the 1σ, 2σ, and 3σ confidence…
Figure 5
Figure 5. Figure 5: Mass and radius diagram for Ross 176 b. There are two world composition models from Zeng et al. 2019: The brown model is an Earth-like planet (30% Fe + 70% MgSiO3), the blue model is a water￾world planet (50% H2O + 50% Earth-like), the navy blue line is a full water-wo…
Figure 6
Figure 6. Figure 6: Interior composition simulation, of Ross 176 b that shows the core, the mantle, the water, and the gas fraction for the planet formation. Left panel: Radius fraction composition. Right panel: Mass fraction composition [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: Synthetic atmospheric transmission spectra of Ross 176 b. Left: Fiducial models for clear or hazy H/He atmospheres with scaled solar abundances. Right: Model for a steam H2O atmosphere. Simulated measurements with error bars are shown for the observation of one (left) …
Figure 8
Figure 8. Figure 8: Eccentricity-orbital period diagram for planets with Rp = 1–3 R⊕. Ross 176 b, HD 40307 b, and Wolf 503 b are overplotted in red, blue, and orange, respectively, following the same criteria as in [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]

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Works this paper leans on

127 extracted references · 58 canonical work pages

  1. [1]

    Abel , M., Frommhold , L., Li , X., & Hunt , K. L. C. 2011, Journal of Physical Chemistry A, 115, 6805

    2011

  2. [2]

    Abel , M., Frommhold , L., Li , X., & Hunt , K. L. C. 2012, , 136, 044319

    2012

  3. [3]

    2012, , 548, A73

    Ag \'u ndez , M., Venot , O., Iro , N., et al. 2012, , 548, A73

    2012

  4. [4]

    L., Chen, X., Ciardi, D., et al

    Akeson, R. L., Chen, X., Ciardi, D., et al. 2013, Publications of the Astronomical Society of the Pacific, 125, 989–999

    2013

  5. [5]

    F., Changeat , Q., Waldmann , I

    Al-Refaie , A. F., Changeat , Q., Waldmann , I. P., & Tinetti , G. 2021, , 917, 37

    2021

  6. [6]

    F., & Barcel \'o Forteza , S

    Aller , A., Lillo-Box , J., Jones , D., Miranda , L. F., & Barcel \'o Forteza , S. 2020, , 635, A128

    2020

  7. [7]

    2015, , 450, 1787

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

    2015

  8. [8]

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

    2007

Show all 127 references
  1. [9]

    E., Mandell , A., Pontoppidan , K., et al

    Batalha , N. E., Mandell , A., Pontoppidan , K., et al. 2017, , 129, 064501

    2017

  2. [10]

    2020, The Astrophysical Journal, 889, 42

    Baumeister, P., Padovan, S., Tosi, N., et al. 2020, The Astrophysical Journal, 889, 42

    2020

  3. [11]

    & Tosi , N

    Baumeister , P. & Tosi , N. 2023, , 676, A106

    2023

  4. [12]

    Bidelman , W. P. 1985, , 59, 197

    1985

  5. [13]

    J., Agol , E., Fressin , F., et al

    Borucki , W. J., Agol , E., Fressin , F., et al. 2013, Science, 340, 587

    2013

  6. [14]

    G., Palumbo , E

    Bouma , L. G., Palumbo , E. K., & Hillenbrand , L. A. 2023, , 947, L3

    2023

  7. [15]

    2021, The Exoplanet Characterization Toolkit (ExoCTK) , Zenodo

    Bourque , M., Espinoza , N., Filippazzo , J., et al. 2021, The Exoplanet Characterization Toolkit (ExoCTK) , Zenodo

    2021

  8. [16]

    2014, , 564, A125

    Buchner , J., Georgakakis , A., Nandra , K., et al. 2014, , 564, A125

    2014

  9. [17]

    A., Cort \'e s-Contreras , M., Alonso-Floriano , F

    Caballero , J. A., Cort \'e s-Contreras , M., Alonso-Floriano , F. J., et al. 2016 a , in 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS19), Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, 148

    2016

  10. [18]

    A., Gu \`a rdia , J., L \'o pez del Fresno , M., et al

    Caballero , J. A., Gu \`a rdia , J., L \'o pez del Fresno , M., et al. 2016 b , in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9910, Observatory Operations: Strategies, Processes, and Systems VI, ed. A. B. Peck , R. L. Seaman , & C. R. Ben...

    2016

  11. [19]

    L., May , E

    Carter , A. L., May , E. M., Espinoza , N., et al. 2024, Nature Astronomy [ [arXiv] 2407.13893 ]

    2024 arXiv

  12. [20]

    2022, , 666, A155

    Chaturvedi , P., Bluhm , P., Nagel , E., et al. 2022, , 666, A155

    2022

  13. [21]

    A., Cort \'e s-Contreras , M., et al

    Cifuentes , C., Caballero , J. A., Cort \'e s-Contreras , M., et al. 2020, , 642, A115

    2020

  14. [22]

    Correia , A. C. M., Bourrier , V., & Delisle , J. B. 2020, , 635, A37

    2020

  15. [23]

    A., Montes , D., et al

    Cort \'e s-Contreras , M., Caballero , J. A., Montes , D., et al. 2024, , 692, A206

    2024

  16. [24]

    M., Wright , E

    Cutri , R. M., Wright , E. L., Conrow , T., et al. 2021, VizieR Online Data Catalog: AllWISE Data Release (Cutri+ 2013) , VizieR On-line Data Catalog: II/328. Originally published in: IPAC/Caltech (2013)

    2013

  17. [25]

    2024, , 968, L22

    Damiano , M., Bello-Arufe , A., Yang , J., & Hu , R. 2024, , 968, L22

    2024

  18. [26]

    & Lichtenberg , T

    Dorn , C. & Lichtenberg , T. 2021, , 922, L4

    2021

  19. [27]

    N., et al

    Dragomir , D., Teske , J., G \"u nther , M. N., et al. 2019, , 875, L7

    2019

  20. [28]

    2018, RNAAS, 2, 209

    Espinoza , N. 2018, RNAAS, 2, 209

    2018

  21. [29]

    2019, , 490, 2262

    Espinoza , N., Kossakowski , D., & Brahm , R. 2019, , 490, 2262

    2019

  22. [30]

    2022, , 163, 133

    Espinoza , N., Pall \'e , E., Kemmer , J., et al. 2022, , 163, 133

    2022

  23. [31]

    P., & Bridges , M

    Feroz , F., Hobson , M. P., & Bridges , M. 2009, , 398, 1601

    2009

  24. [32]

    N., Gustafsson , M., & Orton , G

    Fletcher , L. N., Gustafsson , M., & Orton , G. S. 2018, , 235, 24

    2018

  25. [33]

    2017, AJ, 154, 220

    Foreman-Mackey , D., Agol , E., Angus , R., & Ambikasaran , S. 2017, AJ, 154, 220

    2017

  26. [34]

    J., Mordasini , C., Nettelmann , N., et al

    Fortney , J. J., Mordasini , C., Nettelmann , N., et al. 2013, , 775, 80

    2013

  27. [35]

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

    2018

  28. [36]

    2020, VizieR Online Data Catalog, I/350

    Gaia Collaboration . 2020, VizieR Online Data Catalog, I/350

    2020

  29. [37]

    L., Sarro , L

    Gaia Collaboration , Smart , R. L., Sarro , L. M., et al. 2021, , 649, A6

    2021

  30. [38]

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

    2023

  31. [39]

    & Zhang , X

    Gao , P. & Zhang , X. 2020, , 890, 93

    2020

  32. [40]

    P., Mather, J

    Gardner, J. P., Mather, J. C., Clampin, M., et al. 2006, Space Science Reviews, 123, 485–606

    2006

  33. [41]

    2024, , 685, A147

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

    2024

  34. [42]

    M., Seager , S., Huang , C

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

    2021

  35. [43]

    A., Templeton , M., Terrell , D., et al

    Henden , A. A., Templeton , M., Terrell , D., et al. 2016, VizieR Online Data Catalog: AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016) , VizieR On-line Data Catalog: II/336. Originally published in: 2015AAS...22533616H

    2016

  36. [44]

    V., et al

    H g , E., Fabricius , C., Makarov , V. V., et al. 2000, , 355, L27

    2000

  37. [45]

    X., Vanderburg , A., P \'a l , A., et al

    Huang , C. X., Vanderburg , A., P \'a l , A., et al. 2020 a , Research Notes of the American Astronomical Society, 4, 204

    2020

  38. [46]

    X., Vanderburg , A., P \'a l , A., et al

    Huang , C. X., Vanderburg , A., P \'a l , A., et al. 2020 b , Research Notes of the American Astronomical Society, 4, 206

    2020

  39. [47]

    M., Twicken, J

    Jenkins, J. M., Twicken, J. D., McCauliff, S., et al. 2016, in Software and Cyberinfrastructure for Astronomy IV, ed. G. Chiozzi & J. C. Guzman, Vol. 9913, International Society for Optics and Photonics (SPIE), 99133E

    2016

  40. [48]

    2015, , 576, A78

    Kausch , W., Noll , S., Smette , A., et al. 2015, , 576, A78

    2015

  41. [49]

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

    2018

  42. [50]

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

    2013

  43. [51]

    Kite , E. S. & Ford , E. B. 2018, , 864, 75

    2018

  44. [52]

    2023, , 675, A115

    Korth , J., Gandolfi , D., S ubjak , J., et al. 2023, , 675, A115

    2023

  45. [53]

    2015, PASP, 127, 1161

    Kreidberg , L. 2015, PASP, 127, 1161

    2015

  46. [54]

    H., et al

    Kuzuhara , M., Fukui , A., Livingston , J. H., et al. 2024, , 967, L21

    2024

  47. [55]

    2024, , 692, A238

    Lacedelli , G., Pall \'e , E., Luque , R., et al. 2024, , 692, A238

    2024

  48. [56]

    Lee , J.-M., Heng , K., & Irwin , P. G. J. 2013, , 778, 97

    2013

  49. [57]

    Lee , S. G. 1984, , 89, 702

    1984

  50. [58]

    & Shara , M

    L \'e pine , S. & Shara , M. M. 2005, , 129, 1483

    2005

  51. [59]

    J., et al

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

    2023

  52. [60]

    C., Santerne , A., et al

    Lillo-Box , J., Santos , N. C., Santerne , A., et al. 2022, , 667, A102

    2022

  53. [61]

    & Loeb, A

    Lingam, M. & Loeb, A. 2017, The Astrophysical Journal Letters, 846, L21

    2017

  54. [62]

    & Loeb, A

    Lingam, M. & Loeb, A. 2019, Journal of Cosmology and Astroparticle Physics, 5, 020

    2019

  55. [63]

    2024, Nature Astronomy, 8, 1399

    Luo , H., Dorn , C., & Deng , J. 2024, Nature Astronomy, 8, 1399

    2024

  56. [64]

    J., Kunimoto , M., et al

    Luque , R., Fulton , B. J., Kunimoto , M., et al. 2022 a , , 664, A199

    2022

  57. [65]

    2022 b , , 666, A154

    Luque , R., Nowak , G., Hirano , T., et al. 2022 b , , 666, A154

    2022

  58. [66]

    & Pall \'e , E

    Luque , R. & Pall \'e , E. 2022, Science, 377, 1211

    2022

  59. [67]

    Luyten , W. J. 1957, A catalogue of 9867 stars in the Southern Hemisphere with proper motions exceeding 0.''2 annually

    1957

  60. [68]

    F., et al

    Ma , S., Ito , Y., Al-Refaie , A. F., et al. 2023, , 957, 104

    2023

  61. [69]

    MacDonald , G. J. F. 1964, Reviews of Geophysics and Space Physics, 2, 467

    1964

  62. [70]

    L., Baumeister , P., et al

    MacKenzie , J., Grenfell , J. L., Baumeister , P., et al. 2023, , 671, A65

    2023

  63. [71]

    Mallonn , M., Poppenhaeger , K., Granzer , T., Weber , M., & Strassmeier , K. G. 2022, , 657, A102

    2022

  64. [72]

    Mallorqu \' n , M., B \'e jar , V. J. S., Lodieu , N., et al. 2024, , 689, A132

    2024

  65. [73]

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

    2008

  66. [74]

    M., Montes , D., et al

    Marfil , E., Tabernero , H. M., Montes , D., et al. 2021, VizieR Online Data Catalog, J/A+A/656/A162

    2021

  67. [75]

    I., Travis , L

    Mishchenko , M. I., Travis , L. D., & Mackowski , D. W. 1996, , 55, 535

    1996

  68. [76]

    2021, , 161, 174

    Morello , G., Zingales , T., Martin-Lagarde , M., Gastaud , R., & Lagage , P.-O. 2021, , 161, 174

    2021

  69. [77]

    L., Twicken , J

    Morris , R. L., Twicken , J. D., Smith , J. e. C., et al. 2020, Kepler Data Processing Handbook: Photometric Analysis , Kepler Science Document KSCI-19081-003, id. 6. Edited by Jon M. Jenkins

    2020

  70. [78]

    2021, , 653, A60

    Murgas , F., Astudillo-Defru , N., Bonfils , X., et al. 2021, , 653, A60

    2021

  71. [79]

    2024, , 684, A83

    Murgas , F., Pall \'e , E., Orell-Miquel , J., et al. 2024, , 684, A83

    2024

  72. [80]

    2023, , 680, A73

    Nagel , E., Czesla , S., Kaminski , A., et al. 2023, , 680, A73

    2023

  73. [81]

    2019, Journal of Astronomical Telescopes, Instruments, and Systems, 5, 015001

    Narita , N., Fukui , A., Kusakabe , N., et al. 2019, Journal of Astronomical Telescopes, Instruments, and Systems, 5, 015001

    2019

  74. [82]

    2024, Planetary Systems

    NASA Exoplanet Archive . 2024, Planetary Systems

    2024

  75. [83]

    & Tanaka , Y

    Ohno , K. & Tanaka , Y. A. 2021, , 920, 124

    2021

  76. [84]

    2024, , 689, A179

    Orell-Miquel , J., Murgas , F., Pall \'e , E., et al. 2024, , 689, A179

    2024

  77. [85]

    2023, , 669, A40

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

    2023

  78. [86]

    2023, , 678, A80

    Palle , E., Orell-Miquel , J., Brady , M., et al. 2023, , 678, A80

    2023

  79. [87]

    2022, MuSCAT2\_transit\_pipeline: MuSCAT2 photometry and transit analysis pipelines , Astrophysics Source Code Library, record ascl:2207.013

    Parviainen , H. 2022, MuSCAT2\_transit\_pipeline: MuSCAT2 photometry and transit analysis pipelines , Astrophysics Source Code Library, record ascl:2207.013

    2022

  80. [88]

    R., et al

    Parviainen , H., Palle , E., Zapatero-Osorio , M. R., et al. 2020, , 633, A28

    2020

  81. [89]

    J., et al

    Parviainen , H., Tingley , B., Deeg , H. J., et al. 2019, , 630, A89

    2019

  82. [90]

    M., Reiners , A., Jeffers , S

    Passegger , V. M., Reiners , A., Jeffers , S. V., et al. 2018, , 615, A6

    2018

  83. [91]

    S., Crossfield , I

    Polanski , A. S., Crossfield , I. J. M., Burt , J. A., et al. 2021, , 162, 238

    2021

  84. [92]

    D., Lee , E

    Powell , D., Feinstein , A. D., Lee , E. K. H., et al. 2024, , 626, 979

    2024

  85. [93]

    J., Caballero , J

    Quirrenbach , A., Amado , P. J., Caballero , J. A., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9147, Ground-based and Airborne Instrumentation for Astronomy V, ed. S. K. Ramsay , I. S. McLean , & H. Takami , 91471F

    2014

  86. [94]

    N., Armitage , P

    Raymond , S. N., Armitage , P. J., Moro-Mart \' n , A., et al. 2011, , 530, A62

    2011

  87. [95]

    A., et al

    Reiners , A., Zechmeister , M., Caballero , J. A., et al. 2018, , 612, A49

    2018

  88. [96]

    L., Loyd, R

    Richey-Yowell, T., Shkolnik, E. L., Loyd, R. O. P., et al. 2022, The Astrophysical Journal, 929, 169

    2022

  89. [97]

    R., Winn , J

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

    2015

  90. [98]

    B., Xu, J., Thompson, S

    Rimmer, P. B., Xu, J., Thompson, S. J., et al. 2018, Science Advances, 4, eaar3302

    2018

  91. [99]

    G., Schlichting , H

    Rogers , J. G., Schlichting , H. E., & Young , E. D. 2024, , 970, 47

    2024

  92. [100]

    Rogers , L. A. & Seager , S. 2010, , 716, 1208

    2010

  93. [101]

    Ross , F. E. 1926, , 36, 172

    1926

  94. [102]

    L., Zechmeister , M., Reiners , A., et al

    Ruh , H. L., Zechmeister , M., Reiners , A., et al. 2024, , 692, A138

    2024

  95. [103]

    M., Cifuentes , C., et al

    Schweitzer , A., Passegger , V. M., Cifuentes , C., et al. 2019, , 625, A68

    2019

  96. [104]

    2005, Astrobiology, 5, 706

    Segura, A., Kasting, J., Meadows, V., & et al. 2005, Astrobiology, 5, 706

    2005

  97. [105]

    F., Cutri , R

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

    2006

  98. [106]

    2015, , 576, A77

    Smette , A., Sana , H., Noll , S., et al. 2015, , 576, A77

    2015

  99. [107]

    C., Stumpe , M

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

    2012

  100. [108]

    Speagle , J. S. 2020, , 493, 3132

    2020

  101. [109]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, , 158, 138

    2019

  102. [110]

    G., Oelkers , R

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

    2018

  103. [111]

    C., Smith , J

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

    2014

  104. [112]

    C., Smith , J

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

    2012

  105. [113]

    M., Marfil , E., Montes , D., & Gonz \'a lez Hern \'a ndez , J

    Tabernero , H. M., Marfil , E., Montes , D., & Gonz \'a lez Hern \'a ndez , J. I. 2022, , 657, A66

    2022

  106. [114]

    P., Fortney , J

    Thorngren , D. P., Fortney , J. J., Murray-Clay , R. A., & Lopez , E. D. 2016, , 831, 64

    2016

  107. [115]

    2020, , 636, A74

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

    2020

  108. [116]

    2008, Contemporary Physics, 49, 71

    Trotta, R. 2008, Contemporary Physics, 49, 71

    2008

  109. [117]

    2013, , 549, A48

    Tuomi , M., Anglada-Escud \'e , G., Gerlach , E., et al. 2013, , 549, A48

    2013

  110. [118]

    F., Lee , J

    van Altena , W. F., Lee , J. T., & Hoffleit , E. D. 1995, The general catalogue of trigonometric [stellar] parallaxes

    1995

  111. [119]

    2022, , 926, 150

    Vazan , A., Sari , R., & Kessel , R. 2022, , 926, 150

    2022

  112. [120]

    P., Tinetti , G., Rocchetto , M., et al

    Waldmann , I. P., Tinetti , G., Rocchetto , M., et al. 2015, , 802, 107

    2015

  113. [121]

    Weis , E. W. 1988, , 96, 1710

    1988

  114. [122]

    2021, Nature Astronomy, 5, 822

    Yu , X., He , C., Zhang , X., et al. 2021, Nature Astronomy, 5, 822

    2021

  115. [123]

    & K \"u rster , M

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

    2009

  116. [124]

    , Reiners, A

    Zechmeister, M. , Reiners, A. , Amado, P. J. , et al. 2018, A&A, 609, A12

    2018

  117. [125]

    B., Sasselov , D

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

    2019

  118. [126]

    , " * 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...

  119. [127]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 gl...

Pith tools

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