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KRONOS I: The $1{-}2.8\mu$m JWST Transmission Spectrum of the 23 Myr V1298 Tau c

T0 review · 2 major / 2 minor · reviewed 2026-06-28 · grok-4.3

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Pith's one-line read The 23-Myr-old exoplanet V1298 Tau c shows atmospheric metallicity lower than mature planets of similar mass.

desk verdict New spectrum and H2O detection for this 23-Myr planet, but the metallicity posterior is too broad to support a firm claim of age evolution in the mass-metallicity relation. read the letter →

arxiv 2606.03740 v3 pith:PE2KIEDZ submitted 2026-06-02 astro-ph.EP astro-ph.SR

Matthew M. Murphy , Matthew C. Nixon , Adina D. Feinstein , Luis Welbanks , Girish M. Duvvuri , Saugata Barat , Benjamin V. Rackham , Darryl Z. Seligman
show 11 more authors
Michael Radica Ian J. M. Crossfield Kevin France John H. Livingston Jonathan Lunine Rafael Luque Catriona Murray Sagnick Mukherjee Biruk Nardos Sydney Petz Hinna Shivkumar
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords exoplanetatmospherestransmissionspectroscopyJWSTyoungplanetsatmosphericmetallicityV1298Taucwatervaporsub-Neptunes
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 the JWST NIRISS/SOSS transmission spectrum of V1298 Tau c, a young super-Earth progenitor. Analysis detects water vapor but no other molecules and infers an atmospheric metallicity of roughly 15 times solar. This value aligns with measurements for other young planets yet sits below those reported for mature planets of comparable mass and temperature. The authors interpret the pattern as tentative evidence that the mass-metallicity relation for exoplanets changes with age. A reader would care because the result bears on how planetary atmospheres acquire and retain heavy elements from formation onward.

What carries the argument

Atmospheric retrieval applied to the NIRISS/SOSS transmission spectrum, which extracts molecular volume mixing ratios and the metallicity [O/H] from the strength of absorption features.

What would settle it

A retrieval of the same spectrum that adopts the exact priors, activity corrections, and wavelength range used in a mature-planet study and returns a metallicity consistent with the mature sample would falsify the claimed age evolution.

Watch

Extended reading notes

Core claim

The authors obtain the 1-2.8 micron transmission spectrum of V1298 Tau c and detect H2O with a log10 volume mixing ratio of -1.83 +0.68/-0.77. Retrievals with and without stellar heterogeneity priors both yield an atmospheric metallicity [O/H] of 14.8 +56.0/-12.28 times solar. This metallicity matches values for other young planets, including the outer companion V1298 Tau b, but is systematically lower than metallicities reported for mature planets of similar mass and temperature. The paper therefore concludes that these results supply tentative but growing evidence that the exoplanet mass-metallicity relation evolves with planetary age.

Load-bearing premise

The retrieved [O/H] metallicity can be compared directly to literature values for mature planets without systematic offsets arising from differing retrieval assumptions, stellar activity corrections, or wavelength coverage.

Editorial extensions

If this is right

  • Metallicities measured for young planets remain similar to one another even across a range of planet masses.
  • Mature planets of comparable mass and temperature exhibit higher metallicities than the young sample.
  • Atmospheric metallicity must change after the first few tens of millions of years through ongoing accretion, mixing, or escape.
  • Further transmission spectra of young planets will be required to confirm whether the age trend is general.

Reading between the lines

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

  • Planet-formation models that tie metallicity only to core mass may need an explicit time dimension to match both young and mature observations.
  • Uniform re-analysis of existing young- and mature-planet spectra with identical retrieval setups would test whether the apparent age offset survives removal of methodological differences.
  • If the trend holds, it predicts that even younger planets should display still lower metallicities, a prediction testable with future observations of systems younger than 10 Myr.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 2 minor

Summary. The manuscript presents the 1-2.8 μm JWST NIRISS/SOSS transmission spectrum of the ~23 Myr super-Earth progenitor V1298 Tau c. It reports a detection of H2O with log10 volume mixing ratio -1.83^{+0.68}_{-0.77}, no other molecules, and consistent atmospheric retrievals with and without informed stellar heterogeneity priors. The retrieved metallicity is [O/H] = 14.8^{+56.0}_{-12.28}×solar, stated to be similar to other young planets (including V1298 Tau b) but systematically lower than mature planets of comparable mass and T_eq, providing tentative evidence that the exoplanet mass-metallicity relation evolves with planetary age.

Significance. If the metallicity posterior is robust and the cross-study comparison holds, the result would supply useful constraints on atmospheric evolution or formation pathways as a function of age. A clear strength is the demonstration of consistent retrieval outcomes with and without stellar priors drawn from the observed stellar spectrum. The broad asymmetric uncertainties on [O/H], however, limit the strength of any evolutionary interpretation.

major comments (2)
  1. [Abstract] Abstract: The assertion that the metallicity is 'systematically lower' than literature values for mature planets of similar mass and temperature is not supported by the reported posterior 14.8^{+56.0}_{-12.28}×solar. The lower bound reaches only ~2.5×solar, which overlaps the range of many mature sub-Neptune metallicities; the 'systematically lower' statement therefore depends on the upper tail and requires a quantitative statistical comparison or explicit lower-bound test to remain load-bearing for the evolutionary claim.
  2. [Retrieval results] Retrieval results: The [O/H] value is derived from a single-molecule (H2O) detection over the limited 1-2.8 μm range with the paper's specific cloud/haze and stellar-heterogeneity parameterization. No section demonstrates that this setup produces metallicities on the same scale as the mature-planet retrievals being compared; differing forward-model assumptions, cloud treatments, or wavelength coverage could shift the inferred value by factors of several, directly affecting the central age-evolution claim.
minor comments (2)
  1. The asymmetric uncertainties on [O/H] should be tabulated alongside the young- and mature-planet comparison values to allow readers to assess overlap directly.
  2. Clarify in the text whether the 'informed priors on stellar heterogeneities' test fully addresses activity-induced offsets or only internal consistency.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and valuable comments on our manuscript. We respond to each major comment below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The assertion that the metallicity is 'systematically lower' than literature values for mature planets of similar mass and temperature is not supported by the reported posterior 14.8^{+56.0}_{-12.28}×solar. The lower bound reaches only ~2.5×solar, which overlaps the range of many mature sub-Neptune metallicities; the 'systematically lower' statement therefore depends on the upper tail and requires a quantitative statistical comparison or explicit lower-bound test to remain load-bearing for the evolutionary claim.

    Authors: We agree that the broad and asymmetric uncertainties on the [O/H] posterior result in overlap with some mature-planet values at the lower bound. The abstract statement reflects that the median lies below typical literature values for mature planets of comparable mass and T_eq, supporting the tentative evolutionary interpretation already qualified in the text. We will revise the abstract to explicitly note the lower-bound overlap and qualify the phrasing as 'tentatively lower' while retaining the comparison to the median. A full statistical test across all literature posteriors lies beyond the scope of this work. revision: partial

  2. Referee: [Retrieval results] Retrieval results: The [O/H] value is derived from a single-molecule (H2O) detection over the limited 1-2.8 μm range with the paper's specific cloud/haze and stellar-heterogeneity parameterization. No section demonstrates that this setup produces metallicities on the same scale as the mature-planet retrievals being compared; differing forward-model assumptions, cloud treatments, or wavelength coverage could shift the inferred value by factors of several, directly affecting the central age-evolution claim.

    Authors: We acknowledge that the limited wavelength range and single-molecule constraint, combined with our specific cloud/haze and heterogeneity treatment, could introduce scale differences relative to other studies. Our retrieval follows standard forward-modeling practices used in the broader JWST sub-Neptune literature. We will add a dedicated discussion paragraph in the retrieval results section that explicitly addresses potential systematic offsets arising from wavelength coverage, cloud parameterization, and model assumptions, while reiterating the tentative nature of the age-evolution claim. This addition will qualify the comparison without requiring a full re-analysis of literature data. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity in retrieval-based metallicity measurement

full rationale

The paper's central result is an observational retrieval of [O/H] from the JWST NIRISS/SOSS transmission spectrum of V1298 Tau c, yielding a posterior with large uncertainties. This metallicity is obtained via standard atmospheric retrieval forward modeling with external priors on stellar heterogeneities derived from the observed stellar spectrum; it is not defined in terms of itself, nor does any equation reduce the reported value to a fitted input by construction. The claim of tentative evidence for an evolving mass-metallicity relation rests on direct comparison to independent literature values for other planets, without self-citation chains, uniqueness theorems, or ansatzes that would force the outcome. No load-bearing step matches the enumerated circularity patterns.

Assumptions & free parameters 2 free parameters · 1 assumptions · 0 invented entities

The analysis rests on standard atmospheric retrieval assumptions and two fitted quantities extracted from the spectrum; no new entities are postulated.

free parameters (2)
  • H2O log10 volume mixing ratio = -1.83
    Fitted directly from the transmission spectrum data.
  • atmospheric metallicity [O/H] = 14.8 x solar
    Derived metallicity scaled to solar; central value and asymmetric uncertainties reported.
assumptions (1)
  • domain assumption Standard 1D atmospheric retrieval models accurately recover volume mixing ratios and metallicity from NIRISS/SOSS data when stellar heterogeneities are accounted for.
    Invoked to justify both informed-prior and uninformed retrievals.

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Cite this review

Pith. "Pith review of KRONOS I: The $1{-}2.8\mu$m JWST Transmission Spectrum of the 23 Myr V1298 Tau c." pith.science (2026). https://pith.science/paper/PE2KIEDZ

@misc{pith2026260603740,
  author       = {Pith},
  title        = {Pith review of: KRONOS I: The $1-2.8\mu$m JWST Transmission Spectrum of the 23 Myr V1298 Tau c},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PE2KIEDZ}},
  note         = {Machine review of arXiv:2606.03740}
}
abstract

While recent JWST observations of mature super-Earths and sub-Neptunes have frequently revealed featureless transmission spectra, their inflated progenitors offer a unique window into understanding their primordial compositions. As part of the Keys to Revealing the Origin and Nature Of sub-neptune Systems (KRONOS) JWST program, we present the NIRISS/SOSS transmission spectrum of V1298 Tau c, a $\sim$23 Myr super-Earth progenitor orbiting a young Solar analog. We detect H$_2$O in V1298 Tau c's atmosphere with a $\log_{10}$ volume mixing ratio of $-1.83^{+0.68}_{-0.77}$, but no additional molecules from these data alone. We find consistent results for the planetary atmospheric properties in both retrievals with and without informed priors on stellar heterogeneities based on the observed stellar spectrum. We infer an atmospheric metallicity [O/H] of $14.8^{+56.0}_{-12.28}\times$ the solar value. This metallicity is similar to literature measurements for other young planets, including its massive outer companion V1298~Tau~b. In contrast, this measured metallicity is systematically lower than the metallicities of mature planets of similar mass and temperature. Altogether, these results provide tentative but growing evidence that the exoplanet mass--metallicity relation evolves with planetary age.

Figures

Figures reproduced from arXiv: 2606.03740 by the authors.

Figure 1
Figure 1. The band-integrated (∼0.85–2.83 µm) transit light curve of V1298 Tau c, normalized to the visit median flux, as observed using JWST/NIRISS SOSS on UT 2025 September 6. The transit contact points (t1–t4) are labeled. We see a significantly curved out-of-transit baseline and nu￾merous starspot crossing events (SCEs). ‡ these efforts, best practices for the reduction process are now relatively well known, and the resul… view at source ↗
Figure 2
Figure 2. Detrended light curves and best-fit models of the NIRISS/SOSS Order 1 broadband light curve. Gray points are at the native time cadence of ∼13 s, and black points are binned to ∼5 min cadence. Each panel shows the result of the four methods we implemented to account for stellar surface heterogeneity features in the light curve: 1) masking the features, 2) modeling them as Gaussians, 3) modeling them with fleck, and … view at source ↗
Figure 3
Figure 3. The results of four independent methodologies for handling starspot crossing events during a transit of V1298 Tau c observed with JWST NIRISS/SOSS. Top: The ∼0.8–2.8 µm transmission spectra of V1298 Tau c at a resolution of R=100. The color corresponds to the fitting routine used (see Sections 3.2–3.5). The spectra are manually offset by 21 ppm for Case 1, 20 ppm for Case 3, and 120 ppm for Case 4 to have the same m… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: The 0.8–2.8µm spectrum of V1298 Tau. Top: Comparing the observed spectrum to the best-fit 3-compo￾nent model, and the individual components scaled by their respective covering fractions. Bottom: The corresponding data-model residuals. NIRISS/SOSS is flux calibrated to …
Figure 5
Figure 5. Figure 5: Our fiducial transmission spectrum of V1298 Tau c (black points) compared to the median retrieved models with (blue line) and without (orange line) enforcing informed stellar heterogeneity priors, each binned down to R=100. The 1, 2, and 3σ model uncertainties are illu…
Figure 6
Figure 6. Figure 6: Posterior distributions of key parameters from our atmospheric retrievals with (blue) and without (orange) informed stellar heterogeneity priors, as well as the best-fit pressure-temperature profile. The blue dotted lines illustrate the normal priors applied to fhet, T…
Figure 8
Figure 8. Figure 8: , along with the best-fit retrieved model of S. Barat et al. (2024). The absolute transit depth and rela￾tive depths around the 1.4µm H2O feature are consistent between visits and facilities. As discussed by S. Barat et al. (2024), the HST spec￾trum exhibits relatively…
Figure 9
Figure 9. Figure 9: Results of tests for evening-morning limb asym￾metry on V1298 Tau c. Top: The timing bias spectra from our uniform-limb spectroscopic fits in Cases 1 (blue) and 2 (green), compared to the analytic model (black line) of M. M. Murphy et al. (2024). Bottom: The evening- (…
Figure 10
Figure 10. Figure 10: Placing V1298 Tau c into context with other young and mature exoplanets. Top: atmospheric metallicity versus planet mass. The masses for V1298 Tau bc are from J. H. Livingston et al. (2026). Bottom: bulk density ver￾sus equilibrium temperature. We present systems with…
Figure 11
Figure 11. Figure 11: Top: The transmission spectrum of V1298 Tau c, at a resolution R=50, derived assuming three different limb darkening profiles when fitting the spectroscopic light curves, and enforcing only uniform priors on the coefficients. In each case, we mask all starspot crossin…
Figure 12
Figure 12. Figure 12: Comparing the best-fit logarithmic limb darkening coefficients u1 (top) and u2 (bottom) from Cases 1, 2, and 4 to predictions from ATLAS (solid) and Phoenix (dashed) stellar models. ‡ reflect a difference in where the coefficient profile turns over, as the models pred…
Figure 13
Figure 13. Figure 13: Comparing the best-fit quadratic limb darkening coefficients u1 (top) and u2 (bottom) from Cases 3 to predictions from ATLAS (solid) and Phoenix (dashed) stellar models. ‡ upward slope. At longer wavelengths where the profiles all flatten, the freely fitted coefficien…
Figure 14
Figure 14. Figure 14: Corner plot from our retrieval using informed stellar heterogeneity priors. V1298 Tau not only has a significant magnetic field strength, but that its strength may vary by nearly ∼2× over a few years (B. Finociety et al. 2023). Therefore, the magnetic field of V1298 T…
Figure 15
Figure 15. Figure 15: Corner plot from our retrieval using uninformed stellar heterogeneity priors. C. COLLECTION OF LITERATURE METALLICITIES In Section 8.1, we present a collection of metallicities for mature exoplanets. These are based on a variety of methodologies, and are inferred from…

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Reference graph

Works this paper leans on

203 extracted references · 195 canonical work pages · cited by 1 Pith paper

  1. [1]

    L., et al

    Adams Redai, J., Wogan, N., Wallack, N. L., et al. 2025, AJ, 170, 219, doi: 10.3847/1538-3881/adee92

    work page doi:10.3847/1538-3881/adee92 2025

  2. [2]

    G., Delgado Mena, E., et al

    Adibekyan, V., Sousa, S. G., Delgado Mena, E., et al. 2024, A&A, 683, A159, doi: 10.1051/0004-6361/202348549

    work page doi:10.1051/0004-6361/202348549 2024

  3. [3]

    Escaping Helium and a Highly Muted Spectrum Suggest a Metal-enriched Atmosphere on Sub-Neptune GJ 3090 b from JWST Transit Spectroscopy

    Ahrer, E.-M., Radica, M., Piaulet-Ghorayeb, C., et al. 2025a, ApJL, 985, L10, doi: 10.3847/2041-8213/add010

    work page doi:10.3847/2041-8213/add010

  4. [4]

    , keywords =

    Ahrer, E.-M., Fairman, C., Kirk, J., et al. 2025b, MNRAS, 543, 2442, doi: 10.1093/mnras/staf1535

    work page doi:10.1093/mnras/staf1535

  5. [5]

    2025, Monthly Notices of the Royal Astronomical Society, 540, 2535, doi: 10.1093/mnras/staf819

    Ahrer, E.-M., Gandhi, S., Alderson, L., et al. 2025c, MNRAS, 540, 2535, doi: 10.1093/mnras/staf819

    work page doi:10.1093/mnras/staf819

  6. [6]

    K., Gao , P., Adams Redai , J., et al

    Alam, M. K., Gao, P., Adams Redai, J., et al. 2025, AJ, 169, 15, doi: 10.3847/1538-3881/ad8eb5

    work page doi:10.3847/1538-3881/ad8eb5 2025

  7. [7]

    The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope. III. Single Object Slitless Spectroscopy

    Albert, L., Lafreni` ere, D., Ren´ e, D., et al. 2023, PASP, 135, 075001, doi: 10.1088/1538-3873/acd7a3

    work page doi:10.1088/1538-3873/acd7a3 2023

  8. [8]

    Early Release Science of the exoplanet WASP-39b with JWST NIRSpec G395H

    Alderson, L., Wakeford, H. R., Alam, M. K., et al. 2023, Nature, 614, 664, doi: 10.1038/s41586-022-05591-3

    work page doi:10.1038/s41586-022-05591-3 2023

Show all 203 references
  1. [9]

    E., Wakeford, H

    Alderson, L., Batalha, N. E., Wakeford, H. R., et al. 2024, AJ, 167, 216, doi: 10.3847/1538-3881/ad32c9

    2024 doi

  2. [10]

    H., Espinoza, N., Diamond-Lowe, H., et al

    Allen, N. H., Espinoza, N., Diamond-Lowe, H., et al. 2025, AJ, 170, 240, doi: 10.3847/1538-3881/adfc51

    2025 doi

  3. [11]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481, doi: 10.1146/annurev.astro.46.060407.145222

    2009 doi

  4. [12]

    2006, A&A, 450, 1221, doi: 10.1051/0004-6361:20054040

    Baraffe, I., Alibert, Y., Chabrier, G., & Benz, W. 2006, A&A, 450, 1221, doi: 10.1051/0004-6361:20054040

    2006 doi

  5. [13]

    M., et al

    Barat, S., D´ esert, J.-M., Goyal, J. M., et al. 2024, A&A, 692, A198, doi: 10.1051/0004-6361/202451127

    2024 doi

  6. [14]

    2024, Nature Astronomy, 8, 899, doi: 10.1038/s41550-024-02257-0

    Barat, S., D´ esert, J.-M., Vazan, A., et al. 2024, Nature Astronomy, 8, 899, doi: 10.1038/s41550-024-02257-0

    2024 doi

  7. [15]

    2025, AJ, 170, 165, doi: 10.3847/1538-3881/adec89

    Barat, S., D´ esert, J.-M., Mukherjee, S., et al. 2025, AJ, 170, 165, doi: 10.3847/1538-3881/adec89

    2025 doi

  8. [16]

    G., Mann, A

    Barber, M. G., Mann, A. W., Vanderburg, A., Boyle, A. W., & Lopez Murillo, A. I. 2025, AJ, 170, 32, doi: 10.3847/1538-3881/add7db

    2025 doi

  9. [17]

    J., Strange, J

    Barber, R. J., Strange, J. K., Hill, C., et al. 2014, MNRAS, 437, 1828, doi: 10.1093/mnras/stt2011

    2014 doi

  10. [18]

    V., Col´ on, K., et al

    Barclay, T., Quintana, E. V., Col´ on, K., et al. 2025, arXiv e-prints, arXiv:2502.09730, doi: 10.48550/arXiv.2502.09730

    2025 doi

  11. [19]

    L., Raymond, S

    Bean, J. L., Raymond, S. N., & Owen, J. E. 2021, Journal of Geophysical Research: Planets, 126, doi: 10.1029/2020je006639

    2021 doi

  12. [20]

    G., Welbanks, L., Schlawin, E., et al

    Beatty, T. G., Welbanks, L., Schlawin, E., et al. 2024, ApJL, 970, L10, doi: 10.3847/2041-8213/ad55e9

    2024 doi

  13. [21]

    A., et al

    Bello-Arufe, A., Damiano, M., Bennett, K. A., et al. 2025, ApJL, 980, L26, doi: 10.3847/2041-8213/adaf22

    2025 doi

  14. [22]

    2024, JWST Reveals CH 4, CO2, and H 2O in a Metal-rich Miscible Atmosphere on a Two-Earth-Radius Exoplanet, https://arxiv.org/abs/2403.03325

    Benneke, B., Roy, P.-A., Coulombe, L.-P., et al. 2024, JWST Reveals CH 4, CO2, and H 2O in a Metal-rich Miscible Atmosphere on a Two-Earth-Radius Exoplanet, https://arxiv.org/abs/2403.03325

    2024

  15. [23]

    Berdyugina, S. V. 2005, Living Reviews in Solar Physics, 2, 8, doi: 10.12942/lrsp-2005-8

    2005 doi

  16. [24]

    2023, Monthly Notices of the Royal Astronomical Society, 523, 6282, doi: 10.1093/mnras/stad1873

    Bloot, S., Miguel, Y., Bazot, M., & Howard, S. 2023, Monthly Notices of the Royal Astronomical Society, 523, 6282, doi: 10.1093/mnras/stad1873

    2023 doi

  17. [25]

    J., et al

    Blunt, S., Carvalho, A., David, T. J., et al. 2023, The Astronomical Journal, 166, 62, doi: 10.3847/1538-3881/acde78

    2023 doi

  18. [26]

    2021, The Exoplanet Characterization Toolkit (ExoCTK), 1.0.0 Zenodo, doi: 10.5281/zenodo.4556063

    Bourque, M., Espinoza, N., Filippazzo, J., et al. 2021, The Exoplanet Characterization Toolkit (ExoCTK), 1.0.0 Zenodo, doi: 10.5281/zenodo.4556063

    2021 doi

  19. [27]

    2014, Statistics and Computing, 26, 383–392, doi: 10.1007/s11222-014-9512-y

    Buchner, J. 2014, Statistics and Computing, 26, 383–392, doi: 10.1007/s11222-014-9512-y

    2014 doi

  20. [28]

    2019, Publications of the Astronomical Society of the Pacific, 131, 108005, doi: 10.1088/1538-3873/aae7fc

    Buchner, J. 2019, Publications of the Astronomical Society of the Pacific, 131, 108005, doi: 10.1088/1538-3873/aae7fc

    2019 doi

  21. [29]

    2021, The Journal of Open Source Software, 6, 3001, doi: 10.21105/joss.03001

    Buchner, J. 2021, The Journal of Open Source Software, 6, 3001, doi: 10.21105/joss.03001

    2021 doi

  22. [30]

    2014, A&A, 564, A125, doi: 10.1051/0004-6361/201322971 Ca˜ nas, C

    Buchner, J., Georgakakis, A., Nandra, K., et al. 2014, A&A, 564, A125, doi: 10.1051/0004-6361/201322971 Ca˜ nas, C. I., Lustig-Yaeger, J., Tsai, S.-M., et al. 2026, AJ, 171, 260, doi: 10.3847/1538-3881/ae4976

    2014 doi

  23. [31]

    J., et al

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

    2024 doi

  24. [32]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245, doi: 10.1086/167900

    1989 doi

  25. [33]

    L., May, E

    Carter, A. L., May, E. M., Espinoza, N., et al. 2024, Nature Astronomy, 8, 1008–1019, doi: 10.1038/s41550-024-02292-x The Young Super-Earth Progenitor V1298 Tau c29

    2024 doi

  26. [34]

    Chen, H., & Rogers, L. A. 2016, ApJ, 831, 180, doi: 10.3847/0004-637X/831/2/180

    2016 doi

  27. [35]

    2023, Nature, 620, 292–298, doi: 10.1038/s41586-023-06230-1

    Coulombe, L.-P., Benneke, B., Challener, R., et al. 2023, Nature, 620, 292–298, doi: 10.1038/s41586-023-06230-1

    2023 doi

  28. [36]

    M.-R., Nixon, M

    Davenport, B., Kempton, E. M.-R., Nixon, M. C., et al. 2025, ApJL, 984, L44, doi: 10.3847/2041-8213/adcd76

    2025 doi

  29. [37]

    J., Petigura, E

    David, T. J., Petigura, E. A., Luger, R., et al. 2019a, ApJL, 885, L12, doi: 10.3847/2041-8213/ab4c99

    doi

  30. [38]

    J., Cody, A

    David, T. J., Cody, A. M., Hedges, C. L., et al. 2019b, AJ, 158, 79, doi: 10.3847/1538-3881/ab290f

    doi

  31. [39]

    V., Gillon, M., et al

    Davoudi, F., Rackham, B. V., Gillon, M., et al. 2024, ApJL, 970, L4, doi: 10.3847/2041-8213/ad5c6c de Wit, J., Seager, S., & Niraula, P. 2025, Combined Exoplanet Mass and Atmospheric Characterization for Accelerated Exoplanetology, arXiv, doi: 10.48550/arXiv.2509.25323

    2024 doi

  32. [40]

    Buchhave, L. A. 2023, AJ, 165, 169, doi: 10.3847/1538-3881/acbf39

    2023 doi

  33. [41]

    J., Hutchings, J

    Doyon, R., Willott, C. J., Hutchings, J. B., et al. 2023, PASP, 135, 098001, doi: 10.1088/1538-3873/acd41b

    2023 doi

  34. [42]

    Draine, B. T. 2003, ARA&A, 41, 241, doi: 10.1146/annurev.astro.41.011802.094840

    2003 doi arXiv

  35. [43]

    2021, AJ, 162, 165, doi: 10.3847/1538-3881/ac134d

    Espinoza, N., & Jones, K. 2021, AJ, 162, 165, doi: 10.3847/1538-3881/ac134d

    2021 doi

  36. [44]

    2016, Monthly Notices of the Royal Astronomical Society, 457, 3573–3581, doi: 10.1093/mnras/stw224

    Espinoza, N., & Jord´ an, A. 2016, Monthly Notices of the Royal Astronomical Society, 457, 3573–3581, doi: 10.1093/mnras/stw224

    2016 doi

  37. [45]

    E., Kirk, J., et al

    Espinoza, N., Steinrueck, M. E., Kirk, J., et al. 2024, Nature, 632, 1017, doi: 10.1038/s41586-024-07768-4

    2024 doi

  38. [46]

    2024, Continuing the Legacy of AU Mic: Simultaneous FUV and NIR Observations of AU Mic b,, JWST Proposal

    Feinstein, A., Welbanks, L., Ahrer, E.-M., et al. 2024, Continuing the Legacy of AU Mic: Simultaneous FUV and NIR Observations of AU Mic b,, JWST Proposal. Cycle 3, ID. #5311

    2024

  39. [47]

    2025, Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk,, JWST Proposal

    Feinstein, A., Bergner, J., Barber, M., et al. 2025, Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk,, JWST Proposal. Cycle 4, ID. #8597

    2025

  40. [48]

    D., David, T

    Feinstein, A. D., David, T. J., Montet, B. T., et al. 2022, ApJL, 925, L2, doi: 10.3847/2041-8213/ac4745

    2022 doi

  41. [49]

    D., Montet, B

    Feinstein, A. D., Montet, B. T., Ansdell, M., et al. 2020, AJ, 160, 219, doi: 10.3847/1538-3881/abac0a

    2020 doi

  42. [50]

    D., Montet, B

    Feinstein, A. D., Montet, B. T., Johnson, M. C., et al. 2021, AJ, 162, 213, doi: 10.3847/1538-3881/ac1f24

    2021 doi

  43. [51]

    D., Radica, M., Welbanks, L., et al

    Feinstein, A. D., Radica, M., Welbanks, L., et al. 2023, Nature, 614, 670, doi: 10.1038/s41586-022-05674-1

    2023 doi

  44. [52]

    Feroz, F., & Hobson, M. P. 2008, MNRAS, 384, 449, doi: 10.1111/j.1365-2966.2007.12353.x

    2008 doi

  45. [53]

    P., & Bridges, M

    Feroz, F., Hobson, M. P., & Bridges, M. 2009, MNRAS, 398, 1601, doi: 10.1111/j.1365-2966.2009.14548.x

    2009 doi

  46. [54]

    2010, AJ, 139, 1338, doi: 10.1088/0004-6256/139/4/1338

    Findeisen, K., & Hillenbrand, L. 2010, AJ, 139, 1338, doi: 10.1088/0004-6256/139/4/1338

    2010 doi

  47. [55]

    I., et al

    Finociety, B., Donati, J.-F., Cristofari, P. I., et al. 2023, MNRAS, 526, 4627, doi: 10.1093/mnras/stad3012

    2023 doi

  48. [56]

    2017, AJ, 154, 220, doi: 10.3847/1538-3881/aa9332

    Foreman-Mackey, D., Agol, E., Ambikasaran, S., & Angus, R. 2017, AJ, 154, 220, doi: 10.3847/1538-3881/aa9332

    2017 doi

  49. [57]

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

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306–312, doi: 10.1086/670067

    2013 doi

  50. [58]

    France, K., Loyd, R. O. P., Youngblood, A., et al. 2016, ApJ, 820, 89, doi: 10.3847/0004-637X/820/2/89

    2016 doi

  51. [59]

    2013, ApJ, 766, 81, doi: 10.1088/0004-637X/766/2/81

    Fressin, F., Torres, G., Charbonneau, D., et al. 2013, ApJ, 766, 81, doi: 10.1088/0004-637X/766/2/81

    2013 doi

  52. [60]

    B., et al

    Fu, G., Mukherjee, S., Stevenson, K. B., et al. 2025, ApJL, 989, L17, doi: 10.3847/2041-8213/adf20f

    2025 doi

  53. [61]

    J., Petigura, E

    Fulton, B. J., Petigura, E. A., Howard, A. W., et al. 2017, AJ, 154, 109, doi: 10.3847/1538-3881/aa80eb Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1, doi: 10.1051/0004-6361/201833051

    2017 doi

  54. [62]

    E., & Sari, R

    Ginzburg, S., Schlichting, H. E., & Sari, R. 2016, ApJ, 825, 29, doi: 10.3847/0004-637X/825/1/29

    2016 doi

  55. [63]

    Grankin, K. N. 1999, Astronomy Letters, 25, 526

    1999

  56. [64]

    N., Bouvier, J., Herbst, W., & Melnikov, S

    Grankin, K. N., Bouvier, J., Herbst, W., & Melnikov, S. Y. 2008, A&A, 479, 827, doi: 10.1051/0004-6361:20078476

    2008 doi

  57. [65]

    H., et al

    Gressier, A., Espinoza, N., Allen, N. H., et al. 2024, ApJL, 975, L10, doi: 10.3847/2041-8213/ad73d1

    2024 doi

  58. [66]

    E., Wogan, N., et al

    Gressier, A., Batalha, N. E., Wogan, N., et al. 2025, AJ, 170, 292, doi: 10.3847/1538-3881/ae0929

    2025 doi

  59. [67]

    A., Herczeg, G

    Gully-Santiago, M. A., Herczeg, G. J., Czekala, I., et al. 2017, ApJ, 836, 200, doi: 10.3847/1538-4357/836/2/200

    2017 doi

  60. [68]

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

    2019 doi

  61. [69]

    Gupta, A., & Schlichting, H. E. 2020, MNRAS, 493, 792, doi: 10.1093/mnras/staa315

    2020 doi

  62. [70]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

    2020 doi

  63. [71]

    H., Barman, T., Baron, E., Aufdenberg, J

    Hauschildt, P. H., Barman, T., Baron, E., Aufdenberg, J. P., & Schweitzer, A. 2025, A&A, 698, A47, doi: 10.1051/0004-6361/202554171

    2025 doi

  64. [72]

    2021, AJ, 162, 54, doi: 10.3847/1538-3881/ac06cd

    Hedges, C., Hughes, A., Zhou, G., et al. 2021, AJ, 162, 54, doi: 10.3847/1538-3881/ac06cd

    2021 doi

  65. [73]

    2022, AJ, 163, 143, doi: 10.3847/1538-3881/ac4477

    Hedges, C., Hughes, A., Zhou, G., et al. 2022, AJ, 163, 143, doi: 10.3847/1538-3881/ac4477

    2022 doi

  66. [74]

    W., Marcy, G

    Howard, A. W., Marcy, G. W., Bryson, S. T., et al. 2012, ApJS, 201, 15, doi: 10.1088/0067-0049/201/2/15

    2012 doi

  67. [75]

    W., Sinukoff, E., Blunt, S., et al

    Howard, A. W., Sinukoff, E., Blunt, S., et al. 2025, ApJS, 278, 52, doi: 10.3847/1538-4365/adc5e4

    2025 doi

  68. [76]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55 30Murphy et al. 2026

    2007 doi

  69. [77]

    K., & Schlichting, H

    Inamdar, N. K., & Schlichting, H. E. 2016, ApJL, 817, L13, doi: 10.3847/2041-8205/817/2/L13

    2016 doi

  70. [78]

    P., Davis, T

    Jackson, A. P., Davis, T. A., & Wheatley, P. J. 2012, MNRAS, 422, 2024, doi: 10.1111/j.1365-2966.2012.20657.x

    2012 doi

  71. [79]

    Y., Sohier, O., Venot, O., & Carrasco, N

    Jaziri, A. Y., Sohier, O., Venot, O., & Carrasco, N. 2025, A&A, 701, A33, doi: 10.1051/0004-6361/202555496

    2025 doi

  72. [80]

    M., Lee, J., Kurtz, C., et al

    Jennewein, D. M., Lee, J., Kurtz, C., et al. 2023, in Practice and Experience in Advanced Research

    2023

  73. [81]

    Computing, PEARC ’23 (New York, NY, USA: Association for Computing Machinery), 296–301, doi: 10.1145/3569951.3597573

    doi

  74. [82]

    2014, ApJ, 795, 65, doi: 10.1088/0004-637X/795/1/65

    Jin, S., Mordasini, C., Parmentier, V., et al. 2014, ApJ, 795, 65, doi: 10.1088/0004-637X/795/1/65

    2014 doi

  75. [83]

    C., David, T

    Johnson, M. C., David, T. J., Petigura, E. A., et al. 2022, AJ, 163, 247, doi: 10.3847/1538-3881/ac6271

    2022 doi

  76. [84]

    2020, The Journal of Open Source Software, 5, 2382, doi: 10.21105/joss.02382

    Jones, K., & Espinoza, N. 2020, The Journal of Open Source Software, 5, 2382, doi: 10.21105/joss.02382

    2020 doi

  77. [85]

    A., Blecic, J., Ashtari, R., et al

    Kahle, K. A., Blecic, J., Ashtari, R., et al. 2025, A&A, 701, A184, doi: 10.1051/0004-6361/202554916

    2025 doi

  78. [86]

    E., & Raftery, A

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

    1995 doi

  79. [87]

    K., Lewis, N

    Kataria, T., Sing, D. K., Lewis, N. K., et al. 2016, ApJ, 821, 9, doi: 10.3847/0004-637X/821/1/9

    2016 doi

  80. [88]

    E., Shapiro, A

    Keers, R. E., Shapiro, A. I., Kostogryz, N. M., et al. 2024, ApJL, 977, L7, doi: 10.3847/2041-8213/ad8b51

    2024 doi

  81. [89]

    2026, ApJ, 1000, 220, doi: 10.3847/1538-4357/ae4d3e

    Kimura, T., & Lichtenberg, T. 2026, ApJ, 1000, 220, doi: 10.3847/1538-4357/ae4d3e

    2026 doi

  82. [90]

    S., Fegley, Jr., B., Schaefer, L., & Ford, E

    Kite, E. S., Fegley, Jr., B., Schaefer, L., & Ford, E. B. 2020, ApJ, 891, 111, doi: 10.3847/1538-4357/ab6ffb

    2020 doi

  83. [91]

    M., Shapiro, A

    Kostogryz, N. M., Shapiro, A. I., Witzke, V., et al. 2024, Nature Astronomy, 8, 929, doi: 10.1038/s41550-024-02252-5

    2024 doi

  84. [92]

    2015, PASP, 127, 1161, doi: 10.1086/683602

    Kreidberg, L. 2015, PASP, 127, 1161, doi: 10.1086/683602

    2015 doi

  85. [93]

    1993, Robert Kurucz CD-ROM, 13

    Kurucz, R. 1993, Robert Kurucz CD-ROM, 13

    1993

  86. [94]

    2003, ApJL, 598, L121, doi: 10.1086/380815

    Lammer, H., Selsis, F., Ribas, I., et al. 2003, ApJL, 598, L121, doi: 10.1086/380815

    2003 doi

  87. [95]

    2026, A&A, 709, A272, doi: 10.1051/0004-6361/202659251

    Lavvas, P., Liu, R., Tinetti, G., et al. 2026, A&A, 709, A272, doi: 10.1051/0004-6361/202659251

    2026 doi

  88. [96]

    2023, A&A, 669, A117, doi: 10.1051/0004-6361/202244132

    Leleu, A., Delisle, J.-B., Udry, S., et al. 2023, A&A, 669, A117, doi: 10.1051/0004-6361/202244132

    2023 doi

  89. [97]

    R., & Parmentier, V

    Line, M. R., & Parmentier, V. 2016, ApJ, 820, 78, doi: 10.3847/0004-637X/820/1/78

    2016 doi

  90. [98]

    H., Petigura, E

    Livingston, J. H., Petigura, E. A., David, T. J., et al. 2026, Nature, 649, 310–314, doi: 10.1038/s41586-025-09840-z

    2026 doi

  91. [99]

    D., & Fortney, J

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

    2013 doi

  92. [100]

    J., Edwards, B., Espinoza, N., & Miguel, Y

    Louca, A. J., Edwards, B., Espinoza, N., & Miguel, Y. 2024, Deciphering an Adolescent Warm Sub-Neptune to Unify Formation Models with Primordial Atmospheres,, JWST Proposal. Cycle 3, ID. #6670

    2024

  93. [101]

    J., & Miguel, Y

    Louca, A. J., & Miguel, Y. 2025, ApJ, 991, 121, doi: 10.3847/1538-4357/add736

    2025 doi

  94. [102]

    Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., et al. 2018, ApJ, 867, 70, doi: 10.3847/1538-4357/aae2ae

    2018 doi

  95. [103]

    Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., et al. 2021, ApJ, 907, 91, doi: 10.3847/1538-4357/abd0f0

    2021 doi

  96. [104]

    2025a, A&A, 700, A284, doi: 10.1051/0004-6361/202555580

    Luque, R., Piaulet-Ghorayeb, C., Radica, M., et al. 2025a, A&A, 700, A284, doi: 10.1051/0004-6361/202555580

    doi

  97. [105]

    P., Xue, Q., et al

    Luque, R., Coy, B. P., Xue, Q., et al. 2025b, AJ, 170, 49, doi: 10.3847/1538-3881/addb40

    doi

  98. [106]

    2023, ApJL, 956, L13, doi: 10.3847/2041-8213/acf577

    Madhusudhan, N., Sarkar, S., Constantinou, S., et al. 2023, ApJL, 956, L13, doi: 10.3847/2041-8213/acf577

    2023 doi

  99. [107]

    2009, ApJ, 707, 24, doi: 10.1088/0004-637X/707/1/24

    Madhusudhan, N., & Seager, S. 2009, ApJ, 707, 24, doi: 10.1088/0004-637X/707/1/24

    2009 doi

  100. [108]

    2014, A&A, 573, A90, doi: 10.1051/0004-6361/201423804

    Magic, Z., Chiavassa, A., Collet, R., & Asplund, M. 2014, A&A, 573, A90, doi: 10.1051/0004-6361/201423804

    2014 doi

  101. [109]

    Malsky, I., & Rogers, L. A. 2020, The Astrophysical Journal, 896, 48, doi: 10.3847/1538-4357/ab873f

    2020 doi

  102. [110]

    Maxted, P. F. L. 2018, A&A, 616, A39, doi: 10.1051/0004-6361/201832944

    2018 doi

  103. [111]

    Maxted, P. F. L. 2023, MNRAS, 519, 3723, doi: 10.1093/mnras/stac3741

    2023 doi

  104. [112]

    M., MacDonald, R

    May, E. M., MacDonald, R. J., Bennett, K. A., et al. 2023, ApJL, 959, L9, doi: 10.3847/2041-8213/ad054f

    2023 doi

  105. [113]

    W., Fortenbach, C

    Mayo, A. W., Fortenbach, C. D., Louie, D. R., et al. 2025, AJ, 170, 50, doi: 10.3847/1538-3881/adda2e

    2025 doi

  106. [114]

    L., et al

    Meech, A., Gao, P., Wallack, N. L., et al. 2026, AJ, 171, 274, doi: 10.3847/1538-3881/ae472f

    2026 doi

  107. [115]

    J., de Wit, J., & Rackham, B

    Mercier, S. J., de Wit, J., & Rackham, B. V. 2025, What’s in Your Transit? Towards Reliably Getting 5×More Science from Exoplanet Transit Data, https://arxiv.org/abs/2510.00124

    2025

  108. [116]

    M., & Mazeh, T

    Mills, S. M., & Mazeh, T. 2017, ApJL, 839, L8, doi: 10.3847/2041-8213/aa67eb

    2017 doi

  109. [117]

    Misener, W., & Schlichting, H. E. 2021, MNRAS, 503, 5658, doi: 10.1093/mnras/stab895

    2021 doi

  110. [118]

    E., & Owen, J

    Misener, W., Schulik, M., Schlichting, H. E., & Owen, J. E. 2025, ApJ, 980, 152, doi: 10.3847/1538-4357/ada777

    2025 doi

  111. [119]

    E., Stevenson, K

    Moran, S. E., Stevenson, K. B., Sing, D. K., et al. 2023, ApJL, 948, L11, doi: 10.3847/2041-8213/accb9c

    2023 doi

  112. [120]

    2020, The Journal of Open Source Software, 5, 2103, doi: 10.21105/joss.02103

    Morris, B. 2020, The Journal of Open Source Software, 5, 2103, doi: 10.21105/joss.02103

    2020 doi

  113. [121]

    Morris, B. M. 2020, The Astrophysical Journal, 893, 67, doi: 10.3847/1538-4357/ab79a0

    2020 doi

  114. [122]

    K., Fu, G., et al

    Mukherjee, S., Sing, D. K., Fu, G., et al. 2026, Science, 392, 858, doi: 10.1126/science.adx5903 The Young Super-Earth Progenitor V1298 Tau c31

    2026 doi

  115. [123]

    M., Beatty, T

    Murphy, M. M., Beatty, T. G., & Apai, D. 2024, The Astrophysical Journal, 974, 179, doi: 10.3847/1538-4357/ad7114

    2024 doi

  116. [124]

    M., Beatty, T

    Murphy, M. M., Beatty, T. G., Schlawin, E., et al. 2024, Nature Astronomy, 8, 1562, doi: 10.1038/s41550-024-02367-9

    2024 doi

  117. [125]

    M., Beatty, T

    Murphy, M. M., Beatty, T. G., Schlawin, E., et al. 2025, The Astronomical Journal, 170, 61, doi: 10.3847/1538-3881/addf38

    2025 doi

  118. [126]

    M., Feinstein, A

    Murphy, M. M., Feinstein, A. D., Schochet, M. E., et al. 2026, KRONOS II: Solar-like Umbra and Penumbra Properties on the Young Sun V1298 Tau, https://arxiv.org/abs/2606.16782

    2026

  119. [127]

    A., & Berta-Thompson, Z

    Murray, C. A., & Berta-Thompson, Z. 2026, AJ, 171, 344, doi: 10.3847/1538-3881/ae5b74

    2026 doi

  120. [128]

    A., Chiang, E

    Murray-Clay, R. A., Chiang, E. I., & Murray, N. 2009, ApJ, 693, 23, doi: 10.1088/0004-637X/693/1/23

    2009 doi

  121. [129]

    2025, ApJ, 993, 80, doi: 10.3847/1538-4357/adfe70

    Namekata, K., Maehara, H., Notsu, Y., et al. 2025, ApJ, 993, 80, doi: 10.3847/1538-4357/adfe70

    2025 doi

  122. [130]

    S., Rackham, B

    Narrett, I. S., Rackham, B. V., & de Wit, J. 2024, AJ, 167, 107, doi: 10.3847/1538-3881/ad1f6c

    2024 doi

  123. [131]

    R., Mann, A

    Newton, E. R., Mann, A. W., Kraus, A. L., et al. 2021, AJ, 161, 65, doi: 10.3847/1538-3881/abccc6

    2021 doi

  124. [132]

    V., de Wit, J., et al

    Niraula, P., Rackham, B. V., de Wit, J., et al. 2026, arXiv e-prints, arXiv:2603.24585. https://arxiv.org/abs/2603.24585

    2026

  125. [133]

    C., & Madhusudhan, N

    Nixon, M. C., & Madhusudhan, N. 2020, MNRAS, 496, 269, doi: 10.1093/mnras/staa1150

    2020 doi

  126. [134]

    C., & Madhusudhan, N

    Nixon, M. C., & Madhusudhan, N. 2022, ApJ, 935, 73, doi: 10.3847/1538-4357/ac7c09

    2022 doi

  127. [135]

    C., Welbanks, L., McGill, P., & Kempton, E

    Nixon, M. C., Welbanks, L., McGill, P., & Kempton, E. M.-R. 2024, ApJ, 966, 156, doi: 10.3847/1538-4357/ad354e

    2024 doi

  128. [136]

    C., Somers, R

    Nixon, M. C., Somers, R. S., Savel, A. B., et al. 2025, ApJ, 995, 95, doi: 10.3847/1538-4357/ae17c8 O’Donovan, B., & Bitsch, B. 2026, A&A, 706, A30, doi: 10.1051/0004-6361/202556898

    2025 doi

  129. [137]

    M., Hogg, D

    Oh, S., Price-Whelan, A. M., Hogg, D. W., Morton, T. D., & Spergel, D. N. 2017, AJ, 153, 257, doi: 10.3847/1538-3881/aa6ffd

    2017 doi

  130. [138]

    W., Vazan, A., & Brouwers, M

    Ormel, C. W., Vazan, A., & Brouwers, M. G. 2021, A&A, 647, A175, doi: 10.1051/0004-6361/202039706

    2021 doi

  131. [139]

    P., Bonfanti, A., Gandolfi, D., et al

    Osborn, H. P., Bonfanti, A., Gandolfi, D., et al. 2022, A&A, 664, A156, doi: 10.1051/0004-6361/202243065

    2022 doi

  132. [140]

    C., Boisse, I., et al

    Oshagh, M., Santos, N. C., Boisse, I., et al. 2013, A&A, 556, A19, doi: 10.1051/0004-6361/201321309

    2013 doi

  133. [141]

    E., & Schlichting, H

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

    2024 doi

  134. [142]

    E., & Wu, Y

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

    2013 doi

  135. [143]

    E., & Wu, Y

    Owen, J. E., & Wu, Y. 2017, ApJ, 847, 29, doi: 10.3847/1538-4357/aa890a

    2017 doi

  136. [144]

    L., et al

    Peacock, S., Barman, T., Shkolnik, E. L., et al. 2020, ApJ, 895, 5, doi: 10.3847/1538-4357/ab893a

    2020 doi

  137. [145]

    2024, ApJL, 974, L10, doi: 10.3847/2041-8213/ad6f00

    Piaulet-Ghorayeb, C., Benneke, B., Radica, M., et al. 2024, ApJL, 974, L10, doi: 10.3847/2041-8213/ad6f00

    2024 doi

  138. [146]

    V., Madhusudhan, N., & Apai, D

    Pinhas, A., Rackham, B. V., Madhusudhan, N., & Apai, D. 2018, MNRAS, 480, 5314, doi: 10.1093/mnras/sty2209

    2018 doi

  139. [147]

    2021, MNRAS, 500, 4560, doi: 10.1093/mnras/staa1462

    Poppenhaeger, K., Ketzer, L., & Mallonn, M. 2021, MNRAS, 500, 4560, doi: 10.1093/mnras/staa1462

    2021 doi

  140. [148]

    2019, ApJ, 887, 170, doi: 10.3847/1538-4357/ab55d9

    Powell, D., Louden, T., Kreidberg, L., et al. 2019, ApJ, 887, 170, doi: 10.3847/1538-4357/ab55d9

    2019 doi

  141. [149]

    Rackham, B. V. 2023, speclib, 0.0-beta.0 Zenodo, doi: 10.5281/zenodo.7868050

    2023 doi

  142. [150]

    V., Apai, D., & Giampapa, M

    Rackham, B. V., Apai, D., & Giampapa, M. S. 2018, The Astrophysical Journal, 853, 122

    2018

  143. [151]

    V., Apai, D., & Giampapa, M

    Rackham, B. V., Apai, D., & Giampapa, M. S. 2019, AJ, 157, 96, doi: 10.3847/1538-3881/aaf892

    2019 doi

  144. [152]

    V., & de Wit, J

    Rackham, B. V., & de Wit, J. 2024, AJ, 168, 82, doi: 10.3847/1538-3881/ad5833

    2024 doi

  145. [153]

    V., Iyer, A

    Rackham, B. V., Iyer, A. R., Apai, D., et al. 2026, AJ, 171, 338, doi: 10.3847/1538-3881/ae5f63

    2026 doi

  146. [154]

    2024, The Journal of Open Source Software, 9, 6898, doi: 10.21105/joss.06898

    Radica, M. 2024, The Journal of Open Source Software, 9, 6898, doi: 10.21105/joss.06898

    2024 doi

  147. [155]

    2023, Monthly Notices of the Royal Astronomical Society, 524, 835–856, doi: 10.1093/mnras/stad1762

    Radica, M., Welbanks, L., Espinoza, N., et al. 2023, Monthly Notices of the Royal Astronomical Society, 524, 835–856, doi: 10.1093/mnras/stad1762

    2023 doi

  148. [156]

    2024, ApJL, 962, L20, doi: 10.3847/2041-8213/ad20e4

    Radica, M., Coulombe, L.-P., Taylor, J., et al. 2024, ApJL, 962, L20, doi: 10.3847/2041-8213/ad20e4

    2024 doi

  149. [157]

    2025, ApJL, 979, L5, doi: 10.3847/2041-8213/ada381

    Radica, M., Piaulet-Ghorayeb, C., Taylor, J., et al. 2025, ApJL, 979, L5, doi: 10.3847/2041-8213/ada381

    2025 doi

  150. [158]

    2026, AJ, 171, 314, doi: 10.3847/1538-3881/ae5b9f

    Radica, M., Taylor, J., Rotman, Y., et al. 2026, AJ, 171, 314, doi: 10.3847/1538-3881/ae5b9f

    2026 doi

  151. [159]

    D., Buchhave, L

    Rathcke, A. D., Buchhave, L. A., de Wit, J., et al. 2025, ApJL, 979, L19, doi: 10.3847/2041-8213/ada5c7

    2025 doi

  152. [160]

    E., Rothman, L

    Richard, C., Gordon, I. E., Rothman, L. S., et al. 2012, JQSRT, 113, 1276, doi: 10.1016/j.jqsrt.2011.11.004

    2012 doi

  153. [161]

    E., Madhusudhan, N., Sarkar, S., et al

    Rigby, F. E., Madhusudhan, N., Sarkar, S., et al. 2025, ApJL, 995, L70, doi: 10.3847/2041-8213/ae247d

    2025 doi

  154. [162]

    2024, MNRAS, 531, 1056, doi: 10.1093/mnras/stae984

    Roth, A., Parmentier, V., & Hammond, M. 2024, MNRAS, 531, 1056, doi: 10.1093/mnras/stae984

    2024 doi

  155. [163]

    S., Gordon, I

    Rothman, L. S., Gordon, I. E., Barber, R. J., et al. 2010, JQSRT, 111, 2139, doi: 10.1016/j.jqsrt.2010.05.001

    2010 doi

  156. [164]

    2026, AJ, 171, 263, doi: 10.3847/1538-3881/ae4d3c

    Rotman, Y., McGill, P., Welbanks, L., et al. 2026, AJ, 171, 263, doi: 10.3847/1538-3881/ae4d3c

    2026 doi

  157. [165]

    2026, Nature Astronomy, 10, 371, doi: 10.1038/s41550-025-02723-3

    Roy, P.-A., Benneke, B., Fournier-Tondreau, M., et al. 2026, Nature Astronomy, 10, 371, doi: 10.1038/s41550-025-02723-3

    2026 doi

  158. [166]

    K., Mukherjee, S., et al

    Rustamkulov, Z., Sing, D. K., Mukherjee, S., et al. 2023, Nature, 614, 659, doi: 10.1038/s41586-022-05677-y 32Murphy et al. 2026

    2023 doi

  159. [167]

    R., et al

    Scarsdale, N., Wogan, N., Wakeford, H. R., et al. 2024, AJ, 168, 276, doi: 10.3847/1538-3881/ad73cf

    2024 doi

  160. [168]

    J., et al

    Schlawin, E., Ohno, K., Bell, T. J., et al. 2024a, ApJL, 974, L33, doi: 10.3847/2041-8213/ad7fef

    doi

  161. [169]

    2024b, AJ, 168, 104, doi: 10.3847/1538-3881/ad58e0

    Schlawin, E., Mukherjee, S., Ohno, K., et al. 2024b, AJ, 168, 104, doi: 10.3847/1538-3881/ad58e0

    doi

  162. [170]

    E., & Young, E

    Schlichting, H. E., & Young, E. D. 2022, PSJ, 3, 127, doi: 10.3847/PSJ/ac68e6

    2022 doi

  163. [171]

    P., MacDonald, R

    Schmidt, S. P., MacDonald, R. J., Tsai, S.-M., et al. 2025, AJ, 170, 298, doi: 10.3847/1538-3881/ae019a

    2025 doi

  164. [172]

    Z., Becker, J., Adams, F

    Seligman, D. Z., Becker, J., Adams, F. C., Feinstein, A. D., & Rogers, L. A. 2022, ApJL, 933, L7, doi: 10.3847/2041-8213/ac786e

    2022 doi

  165. [173]

    L., & Barman, T

    Shkolnik, E. L., & Barman, T. S. 2014, AJ, 148, 64, doi: 10.1088/0004-6256/148/4/64

    2014 doi

  166. [174]

    K., Rustamkulov, Z., Thorngren, D

    Sing, D. K., Rustamkulov, Z., Thorngren, D. P., et al. 2024, Nature, 630, 831, doi: 10.1038/s41586-024-07395-z

    2024 doi

  167. [175]

    2006, Bayesian Analysis, 1, 833 , doi: 10.1214/06-BA127

    Skilling, J. 2006, Bayesian Analysis, 1, 833 , doi: 10.1214/06-BA127

    2006 doi

  168. [176]

    Solanki, S. K. 2003, A&A Rv, 11, 153, doi: 10.1007/s00159-003-0018-4 Solov’ev, A. A., & Kirichek, E. A. 2019, MNRAS, 482, 5290, doi: 10.1093/mnras/sty3050

    2003 doi

  169. [177]

    R., Jones, B

    Stauffer, J. R., Jones, B. F., Backman, D., et al. 2003, AJ, 126, 833, doi: 10.1086/376739

    2003 doi

  170. [178]

    Steinmeyer, M.-L., Dorn, C., Werlen, A., & Grimm, S. L. 2026, ApJ, 1001, 36, doi: 10.3847/1538-4357/ae4c47 Su´ arez Mascare˜ no, A., Damasso, M., Lodieu, N., et al. 2021, Nature Astronomy, 6, 232, doi: 10.1038/s41550-021-01533-7

    2026 doi

  171. [179]

    X., Welbanks, L., Teske, J., & Buchner, J

    Sun, Q., Wang, S. X., Welbanks, L., Teske, J., & Buchner, J. 2024, AJ, 167, 167, doi: 10.3847/1538-3881/ad298d S¨ utterlin, P., Wiehr, E., & Stellmacher, G. 1999, SoPh, 189, 57, doi: 10.1023/A:1005243302461

    2024 doi

  172. [180]

    R., Hasegawa, Y., Thorngren, D

    Swain, M. R., Hasegawa, Y., Thorngren, D. P., & Roudier, G. M. 2024, Space Science Reviews, 220, doi: 10.1007/s11214-024-01098-7

    2024 doi

  173. [181]

    D., et al

    Taylor, J., Radica, M., Chatterjee, R. D., et al. 2025, MNRAS, 540, 3677, doi: 10.1093/mnras/staf894

    2025 doi

  174. [182]

    E., Wallack, N

    Teske, J., Batalha, N. E., Wallack, N. L., et al. 2025, AJ, 169, 249, doi: 10.3847/1538-3881/adb975

    2025 doi

  175. [183]

    K., Wallack, N

    Teske, J. K., Wallack, N. L., Piette, A. A. A., et al. 2025, ApJL, 995, L39, doi: 10.3847/2041-8213/ae0a4c

    2025 doi

  176. [184]

    C., Mann, A

    Thao, P. C., Mann, A. W., Feinstein, A. D., et al. 2024, AJ, 168, 297, doi: 10.3847/1538-3881/ad81d7

    2024 doi

  177. [185]

    Lopez, E. D. 2016, ApJ, 831, 64, doi: 10.3847/0004-637X/831/1/64

    2016 doi

  178. [186]

    2008, Contemporary Physics, 49, 71, doi: 10.1080/00107510802066753

    Trotta, R. 2008, Contemporary Physics, 49, 71, doi: 10.1080/00107510802066753

    2008 doi

  179. [187]

    Valatsou, M., Dorn, C., Marty, P., & Owen, J. E. 2026, arXiv e-prints, arXiv:2602.12201, doi: 10.48550/arXiv.2602.12201

    2026 doi arXiv

  180. [188]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261, doi: 10.1038/s41592-019-0686-2

    2020 doi

  181. [189]

    K., Diamond-Lowe, H., et al

    Wachiraphan, P., Berta-Thompson, Z. K., Diamond-Lowe, H., et al. 2025, AJ, 169, 311, doi: 10.3847/1538-3881/adc990

    2025 doi

  182. [190]

    L., Gao, P., Greklek-McKeon, M., et al

    Wallack, N. L., Gao, P., Greklek-McKeon, M., et al. 2026, AJ, 171, 180, doi: 10.3847/1538-3881/ae2d12

    2026 doi

  183. [191]

    R., et al

    Wang, H., Spirock, T., Goode, P. R., et al. 1998, ApJ, 495, 957, doi: 10.1086/305311

    1998 doi

  184. [192]

    K., et al

    Wang, L.-C., Rustamkulov, Z., Sing, D. K., et al. 2026, AJ, 171, 147, doi: 10.3847/1538-3881/ae231b

    2026 doi

  185. [193]

    2021, ApJ, 913, 114, doi: 10.3847/1538-4357/abee94

    Welbanks, L., & Madhusudhan, N. 2021, ApJ, 913, 114, doi: 10.3847/1538-4357/abee94

    2021 doi

  186. [194]

    F., et al

    Welbanks, L., Madhusudhan, N., Allard, N. F., et al. 2019, ApJL, 887, L20, doi: 10.3847/2041-8213/ab5a89

    2019 doi

  187. [195]

    J., Beatty, T

    Welbanks, L., Bell, T. J., Beatty, T. G., et al. 2024, Nature, 630, 836–840, doi: 10.1038/s41586-024-07514-w

    2024 doi

  188. [196]

    C., McGill, P., et al

    Welbanks, L., Nixon, M. C., McGill, P., et al. 2025, Nature Astronomy, 10, 234–247, doi: 10.1038/s41550-025-02730-4

    2025 doi

  189. [197]

    2025, ApJL, 991, L16, doi: 10.3847/2041-8213/adff73

    Werlen, A., Dorn, C., Burn, R., et al. 2025, ApJL, 991, L16, doi: 10.3847/2041-8213/adff73

    2025 doi

  190. [198]

    Wichmann, R., Krautter, J., Schmitt, J. H. M. M., et al. 1996, A&A, 312, 439

    1996

  191. [199]

    F., Batalha, N

    Wogan, N. F., Batalha, N. E., Zahnle, K. J., et al. 2024, ApJL, 963, L7, doi: 10.3847/2041-8213/ad2616

    2024 doi

  192. [200]

    Yelle, R. V. 2004, Icarus, 170, 167, doi: 10.1016/j.icarus.2004.02.008

    2004 doi

  193. [201]

    N., Barber, R

    Yurchenko, S. N., Barber, R. J., & Tennyson, J. 2011, MNRAS, 413, 1828, doi: 10.1111/j.1365-2966.2011.18261.x

    2011 doi

  194. [202]

    N., & Tennyson, J

    Yurchenko, S. N., & Tennyson, J. 2014, MNRAS, 440, 1649, doi: 10.1093/mnras/stu326

    2014 doi

  195. [203]

    J., & Catling, D

    Zahnle, K. J., & Catling, D. C. 2017, ApJ, 843, 122, doi: 10.3847/1538-4357/aa7846

    2017 doi

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