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REVIEW 3 major objections 5 minor 85 references

LRG-BEASTS: transmission spectroscopy and retrieval analysis of the highly-inflated Saturn-mass planet WASP-39b

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read A retrieval of all published spectra of WASP-39b yields a 282-times-solar metallicity and attributes previous contradictions to retrieval assumptions.

desk verdict A solid new ground-based spectrum and a useful uniform re-analysis of all WASP-39b data, but the headline 282x solar metallicity is not secured against the isothermal T-P bias the paper itself flags. read the letter →

arxiv 1908.02358 v2 pith:M7SXEKXZ submitted 2019-08-06 astro-ph.EP

James Kirk , Mercedes Lopez-Morales , Peter J. Wheatley , Ian C. Weaver , Ian Skillen , Tom Louden , James McCormac , Nestor Espinoza This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetatmospherestransmissionspectroscopyWASP-39batmosphericmetallicityretrievalanalysisequilibriumchemistryhotSaturnground-basedobservations
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 a new ground-based transmission spectrum of the hot Saturn-mass exoplanet WASP-39b, taken at low resolution with the 4.2 m William Herschel Telescope, and reanalyzes every previously published spectrum of the planet with a single retrieval framework. Running a retrieval code that assumes equilibrium chemistry on all data sets, the authors recover an atmosphere that is consistently very metal-rich, with the combined spectrum giving a metallicity of $282^{+65}_{-58}\times$ solar. They argue that the four-orders-of-magnitude scatter in earlier water-abundance measurements comes from different retrieval assumptions, such as reference pressure, radius, priors, and treatment of the temperature profile, and not from stellar activity or bad data. If the central claim is right, WASP-39b's atmosphere is more metal-rich than current interior-evolution models allow, which would challenge standard ideas about how such planets form and evolve.

What carries the argument

The argument runs on the platon atmospheric retrieval code, which assumes equilibrium chemistry and an isothermal temperature-pressure profile and parametrizes clouds and hazes through cloud-top pressure, a scattering-slope scale factor, and a scattering gradient; parameters are explored with nested sampling. Water is the metallicity tracer: under equilibrium chemistry, the water abundance is set by the metallicity and the C/O ratio, so the amplitude of the 1.4 micron water feature carries the abundance measurement. The key dataset is the combined transmission spectrum from 0.29 to 5.06 microns, built by merging the new WHT/ACAM optical points with HST/STIS, VLT/FORS, HST/WFC3, and Spitzer/IRAC measurements; the optical data supply a pressure reference that helps break the degeneracy between water abundance, reference radius, and cloud-top pressure.

What would settle it

Run the same retrieval on the combined spectrum using a non-isothermal, parametrized temperature-pressure profile rather than an isothermal one; if the retrieved metallicity drops below roughly $54.5\times$ solar or the water abundance falls to subsolar values, the central claim fails. A direct secondary-eclipse measurement of the thermal emission would also test whether the atmosphere is actually isothermal.

Watch

Extended reading notes

Core claim

The central claim is that previous disagreements about WASP-39b's water abundance, which span more than four orders of magnitude, are retrieval artifacts rather than astrophysical or data-quality problems. Applying one retrieval framework that assumes equilibrium chemistry to every existing spectrum, including two independent reductions of the same HST/WFC3 data that had previously yielded subsolar and supersolar answers, produces supersolar metallicities in all cases. For the combined spectrum across 0.3 to 5 microns, the retrieved metallicity is $282^{+65}_{-58}\times$ solar, with a C/O ratio consistent with solar. The paper also claims that stellar activity changes the answer only negligibly, and that the 282-times-solar value, if true, exceeds the maximal atmospheric metallicity of $54.5\times$ solar allowed by current interior models.

Load-bearing premise

The result rests on assuming the planet's temperature is the same at all altitudes; the paper itself notes that if that assumption is wrong, retrieved metal abundances can be inflated by about tenfold.

Editorial extensions

If this is right

  • If the metallicity is really 282 times solar, WASP-39b violates the current interior-model ceiling of about 54.5 times solar, so either the planet's interior is hotter, younger, or tidally heated, or the atmosphere has been enriched after formation.
  • Stellar activity can be ruled out as the cause of the order-of-magnitude abundance scatter, simplifying the interpretation of similar hot Saturn and hot Jupiter spectra.
  • Combining optical and infrared data within a common retrieval framework yields consistent supersolar metallicities for every data set, so future WASP-39b work should analyze all available epochs together.
  • Four-meter-class ground-based telescopes can deliver transmission spectra with roughly one-scale-height precision, meaning they can support space-based observatories by screening targets and extending wavelength coverage.
  • The same retrieval-assumption biases will apply to JWST abundance measurements of smaller planets, so standardizing the treatment of temperature profiles, reference radii, and priors is necessary before claiming precise abundances.

Reading between the lines

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

  • If the isothermal bias quantified in other retrieval studies applies here, the true metallicity may fall closer to the 10 to 50 times solar range, which would reconcile the atmosphere with interior-model limits; a non-isothermal retrieval of the combined spectrum can test this directly.
  • The paper's diagnosis implies that water-abundance measurements of hot Jupiters from single-grism HST data alone are not robust, and a standardized multi-instrument, multi-epoch retrieval protocol could remove most of the reported spread across the literature.
  • The muted sodium and potassium wings, which the paper attributes to possible alkali chloride condensation, could be checked with high-resolution spectra of the alkali line cores: condensation predicts narrow cores without broad pressure wings at a specific temperature.
  • A natural extension is to treat inter-instrument transit-depth offsets as free parameters in the joint retrieval instead of normalizing them away, which would quantify the systematic uncertainty in the 282-times-solar value.
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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 / 5 minor

Summary. WASP-39b is a highly inflated Saturn-mass planet with conflicting published water abundances spanning four orders of magnitude. The paper presents a new ground-based WHT/ACAM low-resolution transmission spectrum (R~400, 4000-9000 Å) from a single transit, reduced with careful Gaussian-process light-curve fitting. It assembles a combined spectrum from HST/STIS, VLT/FORS, HST/WFC3 (two reductions), Spitzer/IRAC, and the new WHT data, and runs platon retrievals that assume isothermal temperature-pressure profiles and equilibrium chemistry. All datasets return supersolar metallicities; the combined retrieval gives 282+65-58 x solar, and stellar activity is found to have negligible effect. The paper concludes that the literature discrepancy is due to retrieval assumptions rather than stellar activity or data quality.

Significance. If the 282x solar metallicity is correct, WASP-39b would join a small set of highly super-solar exoplanet atmospheres and would challenge interior-structure upper limits (Thorngren & Fortney 2019, 54.5x solar), with implications for formation via icy planetesimal accretion. The paper's strengths are its careful, transparent light-curve analysis (GP detrending, limb-darkening from stellar models, direct comparison with earlier VLT/HST binning), its uniform application of one retrieval code to all literature datasets, and its explicit tabulation of the combined spectrum. The weaknesses are model-dependent: the headline number rests on the isothermal and equilibrium-chemistry assumptions, both of which the paper identifies as potentially large biases. The significance is accordingly conditional on resolving those assumptions.

major comments (3)
  1. [Section 6, Table 5; Section 7.1] The headline metallicity of 282+65-58x solar (Table 5) is not secured against the isothermal temperature-pressure assumption. The paper itself states in Section 7.1 that platon cannot yet perform non-isothermal retrievals on transmission spectra and cites Rocchetto et al. (2016), who found that assuming an isothermal profile can bias retrieved abundances an order of magnitude high with underestimated uncertainties. Since every retrieval in Table 5 uses an isothermal profile, the quoted metallicities could be systematically high. The counterargument that published abundances do not correlate cleanly with T-P treatment conflates changes in code, data, priors, and chemistry, and is not a substitute for a test on the datasets used here. I request a non-isothermal retrieval with an independent code, or explicit simulations showing that the isothermal bias is small for the WASP-39b data.
  2. [Section 8 vs Section 7.1, Table 5] The conclusion (Section 8) that the literature discrepancies are 'more likely due to differing retrieval approaches, in particular the treatment of the reference pressure and planetary radius' is contradicted by the paper's own test. In Section 7.1 the authors fix the reference radius and cloud-top pressure to the Tsiaras et al. (2018) values and still recover logZ = 2.72+0.11-0.12 and 2.74+0.11-0.10 (Table 5), i.e., still highly supersolar. Thus the fixed reference-pressure test does not reconcile the abundance, and it was performed only on the T18 dataset, not on the combined spectrum used for the 282x claim. This attribution should be removed or revised.
  3. [Section 6, Section 7.1] The equilibrium-chemistry assumption is also untested within the authors' framework. platon assumes equilibrium chemistry, and the paper states that a free-chemistry analysis is future work. The only evidence cited against chemistry as the driver is Wakeford et al. (2018)'s disequilibrium value of 117+14-30x solar, obtained with a different retrieval code and prior setup; it does not establish the robustness of 282x solar to the chemistry assumption. A free-chemistry retrieval of the combined spectrum, or an explicit sensitivity test, is needed before the paper can claim that the literature spread stems from retrieval assumptions rather than chemistry.
minor comments (5)
  1. [Table 3] The table's wavelength ordering is non-monotonic (e.g., 0.9625 µm appears before 0.9572 µm), which makes it difficult to scan; please reorder rows by increasing wavelength.
  2. [Figure 6] The legend entry '0p1X solar' appears to be a typo for '0.1X solar'; please correct.
  3. [Table 5] The labels 'T18 w/o activity' with and without the fixed reference radius are confusing; consider renaming the fixed entries, e.g., 'T18 w/o activity, fixed RP and Pcloud'.
  4. [Section 5.2] The phrase 'this data' (used for 'this work') should be 'these data' for consistency.
  5. [Section 7.1] The sentence that the discrepancies 'could be related to a degeneracy between the reference pressure, reference radius and the abundance of water' is immediately followed by the Welbanks & Madhusudhan (2019) result that this degeneracy has little effect on abundance estimates; please resolve this tension explicitly.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the 282x solar metallicity is a directly fitted retrieval output from an external code and independent data sets, not a predicted quantity forced by the model inputs.

full rationale

The central claim is a retrieved (fitted) atmospheric metallicity produced by the externally maintained platon retrieval code (Zhang et al. 2019) acting on measured transmission spectra, with model parameters and priors stated in Section 6 and Table 4. The quoted 282+65/-58x solar value is the posterior mode of a nested-sampling fit, not a quantity derived from a first-principles chain that is definitionally equivalent to its inputs. The paper's re-analysis of literature data sets is a controlled comparison using the same code and assumptions, not a prediction of those data from the fitted value. The isothermal temperature-pressure assumption is explicitly acknowledged in Section 7.1 with an external caveat from Rocchetto et al. (2016); this is a model-dependence and correctness risk, not circularity. Self-citations (Kirk et al. 2017, 2018; Louden et al. 2017; Kirk 2018) concern observational reduction methodology and previous LRG-BEASTS targets, and are not load-bearing for the supersolar metallicity conclusion. No equation is shown to reduce to its own input, and no fitted parameter is renamed as a prediction. The paper is self-contained against external benchmarks in the sense that the retrieval is benchmarked against independent data and an independent code (atmo), so the circularity score is 0.

Assumptions & free parameters 10 free parameters · 5 assumptions · 0 invented entities

The central claim rests on the platon retrieval's assumptions: equilibrium chemistry, an isothermal T-P profile, cloud and haze parameterization, and the normalization of optical to infrared data. These assumptions are not independently verified in this paper, and the isothermal assumption is cited as capable of order-of-magnitude abundance biases.

free parameters (10)
  • Atmospheric metallicity log Z = 2.45 (282x solar, combined with activity)
    Central retrieved parameter; determines the headline claim.
  • Planet radius at 1 bar RP = 1.20 RJ
    Retrieved parameter; degenerates with abundances and pressure reference.
  • Equilibrium temperature Teq = 1133 K
    Retrieved parameter; sets the atmospheric scale height.
  • C/O ratio = 0.25
    Retrieved parameter; discussed in the formation context.
  • Cloud-top pressure log Pcloud = -2.17 bar
    Retrieved parameter; controls the optical transmission slope.
  • Scattering factor log s = -2.51
    Retrieved parameter; adjusts the Rayleigh scattering slope amplitude.
  • Scattering gradient alpha = 4.07
    Retrieved parameter; controls the spectral slope gradient.
  • Active region temperature T_active = 3257 K
    Retrieved parameter; poorly constrained stellar activity parameter.
  • Active region covering fraction f_active = 0.05
    Retrieved parameter; poorly constrained.
  • Optical-to-infrared normalization offset = not reported, per data set
    The paper subtracts mean transit depth differences to align optical and IR data for single-optical retrievals; this data-derived correction can affect the slope and retrieved abundances.
assumptions (5)
  • domain assumption Equilibrium chemistry for all molecular abundances
    platon assumes chemical equilibrium; the paper states 'Our retrievals, which assume equilibrium chemistry' and does not test free chemistry with platon.
  • ad hoc to paper Isothermal temperature-pressure profile
    platon does not support non-isothermal T-P profiles for transmission retrievals (Section 7.1); Rocchetto et al. (2016) is cited showing this can bias abundances high.
  • domain assumption Clouds and hazes parameterized as gray cloud top plus power-law scattering
    The retrieval fits log Pcloud, log s, and alpha to represent aerosols; this is a simplified parameterization, not a microphysical model.
  • domain assumption Stellar activity has negligible effect on infrared transit spectra
    The paper cites Rackham et al. (2018) for FGK dwarfs; this motivates normalizing optical data to IR and modeling activity only with a spot or facula parameterization.
  • ad hoc to paper Mean transit depth offsets between instruments can be removed by subtracting mean differences
    For single optical data sets, the authors subtract the mean transit depth difference relative to WFC3; a constant offset in depth can create or remove spectral slopes.

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Cite this review

Pith. "Pith review of LRG-BEASTS: transmission spectroscopy and retrieval analysis of the highly-inflated Saturn-mass planet WASP-39b." pith.science (2026). https://pith.science/paper/M7SXEKXZ

@misc{pith2026190802358,
  author       = {Pith},
  title        = {Pith review of: LRG-BEASTS: transmission spectroscopy and retrieval analysis of the highly-inflated Saturn-mass planet WASP-39b},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/M7SXEKXZ}},
  note         = {Machine review of arXiv:1908.02358}
}
abstract

We present a ground-based transmission spectrum and comprehensive retrieval analysis of the highly inflated Saturn-mass planet WASP-39b. We obtained low-resolution spectra ($R \approx 400$) of a transit of WASP-39b using the ACAM instrument on the 4.2m William Herschel Telescope as part of the LRG-BEASTS survey. Our transmission spectrum is in good agreement with previous ground- and space-based observations of WASP-39b, and covers a wavelength range of 4000-9000A. Previous analyses of this exoplanet have retrieved water abundances that span more than four orders of magnitude, which in turn lead to conclusions of a subsolar or highly supersolar atmospheric metallicity. In order to determine the cause of the large discrepancies in the literature regarding WASP-39b's atmospheric metallicity, we performed retrieval analyses of all literature data sets. Our retrievals, which assume equilibrium chemistry, recovered highly supersolar metallicities for all data sets. When running our retrievals on a combined spectrum, spanning 0.3-5$\mu$m, we recovered an atmospheric metallicity of $282^{+65}_{-58} \times$ solar. We find that stellar activity has a negligible effect on the derived abundances and instead conclude that different assumptions made during retrieval analyses lead to the reported water abundances that differ by orders of magnitude. This in turn has significant consequences for the conclusions we draw. This is the fourth planet to be observed as part of the LRG-BEASTS survey, which is demonstrating that 4m class telescopes can obtain low-resolution transmission spectra with precisions of around one atmospheric scale height.

Figures

Figures reproduced from arXiv: 1908.02358 by the authors.

Figure 1
Figure 1. Top panel: image taken through the 4000 slit. WASP-39 is the left-hand bright star, and the comparison is the right-hand bright star. This panel is cropped vertically. Bottom panel: an example science frame. WASP-39 is the left-hand bright trace, and the comparison is the right-hand bright trace. The solid blue lines show the target aperture, and the dashed lines indicate the region over which the background was cal… view at source ↗
Figure 2
Figure 2. Diagnostic plots of the night’s data, all plotted with time on the x-axis. Top panel: variation of air mass across the observations. Second panel: the shift in the target’s spectrum (blue crosses) and comparison’s spectrum (red pluses) along the spatial direction. Third panel: the shift in the target’s spectrum (blue crosses) and comparison’s spectrum (red pluses) along the dispersion direction. Fourth panel: rotati… view at source ↗
Figure 3
Figure 3. Normalized spectra of the target (blue line) and comparison (red line). The black dashed vertical lines show the wavelength bins used to generate the spectroscopic light curves. The green vertical lines show the location of the sodium and potassium features, which are both encompassed within narrow bins (30 and 50 ˚A respectively). Wavelengths outside of the range 4000–9000 ˚A were excluded due to low signal to nois… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Plot of the fit using an analytic transit light curve and Gaussian process to the white-light curve of WASP-39. Top panel: the data are shown by the black error bars with the best-fitting model shown in red. The green line and gray dashed lines show the contributions o…
Figure 5
Figure 5. Figure 5: Left-hand panel: fits to our spectroscopic light curves combining quadratically limb-darkened analytic transit light curves with a GP. The black data points show the transit light curve for each wavelength bin, with the central wavelength of each bin given on the right…
Figure 6
Figure 6. Figure 6: Our WHT transmission spectrum with forward models overplotted. The green and yellow models were generated using exo-transmit and correspond to subsolar and solar atmospheres with Rayleigh scattering slopes enhanced by factors of 15 and 10, respectively. The blue line c…
Figure 7
Figure 7. Figure 7: Top panel: a comparison between the transmission spectrum resulting from our WHT/ACAM data (black error bars) and the transmission spectrum resulting from Nikolov et al. (2016)’s VLT/FORS data (red error bars). Middle panel: a comparison between the transmission spectr…
Figure 8
Figure 8. Figure 8: Results from the running of platon retrievals. Each panel is labeled according to which combination of data sets is used. In each panel, the black points show the data, the solid red line shows the retrieved model without accounting for stellar activity, and the blue l…
Figure 9
Figure 9. Figure 9: The platon retrievals run on the combined transmission spectrum, incorporating data from five different studies ( [PITH_FULL_IMAGE:figures/full_fig_p018_9.png]

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Works this paper leans on

85 extracted references · 8 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ""...

  3. [3]

    On detecting terrestrial planets with timing of giant planet transits

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    work page Pith review arXiv 2017

  4. [4]

    Aigrain , S., Parviainen , H., & Pope , B. J. S. 2016, , 459, 2408, 10.1093/mnras/stw706

    doi:10.1093/mnras/stw706 2016

  5. [5]

    W., & O'Neil , M

    Ambikasaran , S., Foreman-Mackey , D., Greengard , L., Hogg , D. W., & O'Neil , M. 2014, ArXiv e-prints. 1403.6015

    arXiv 2014

  6. [6]

    R., et al

    Arcangeli , J., Desert , J.-M., Line , M. R., et al. 2018, ArXiv e-prints. 1801.02489

    arXiv 2018

  7. [7]

    J., de Mooij , E., Barstow , J., et al

    Armstrong , D. J., de Mooij , E., Barstow , J., et al. 2016, Nature Astronomy, 1, 0004, 10.1038/s41550-016-0004

    doi:10.1038/s41550-016-0004 2016

  8. [8]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

Show all 85 references
  1. [9]

    K., Aigrain , S., Irwin , P

    Barstow , J. K., Aigrain , S., Irwin , P. G. J., & Sing , D. K. 2017, , 834, 50, 10.3847/1538-4357/834/1/50

    2017 doi

  2. [10]

    2008, in , Vol

    Benn , C., Dee , K., & Ag \'o cs , T. 2008, in , Vol. 7014, Ground-based and Airborne Instrumentation for Astronomy II, 70146X

    2008

  3. [11]

    2012, , 753, 100, 10.1088/0004-637X/753/2/100

    Benneke , B., & Seager , S. 2012, , 753, 100, 10.1088/0004-637X/753/2/100

    2012 doi

  4. [12]

    2015, The Messenger, 159, 6

    Boffin , H., Blanchard , G., Gonzalez , O., et al. 2015, The Messenger, 159, 6. 1502.03172

    2015 arXiv

  5. [13]

    K., Stevenson , K

    Bruno , G., Lewis , N. K., Stevenson , K. B., et al. 2018, , 156, 124, 10.3847/1538-3881/aac6db

    2018 doi

  6. [14]

    Burrows , A., & Sharp , C. M. 1999, , 512, 843, 10.1086/306811

    1999 doi

  7. [15]

    M., Noyes , R

    Charbonneau , D., Brown , T. M., Noyes , R. W., & Gilliland , R. L. 2002, , 568, 377, 10.1086/338770

    2002 doi

  8. [16]

    Crossfield , I. J. M., & Kreidberg , L. 2017, , 154, 261, 10.3847/1538-3881/aa9279

    2017 doi

  9. [17]

    2016, , 457, 3573, 10.1093/mnras/stw224

    Espinoza , N., & Jord \'a n , A. 2016, , 457, 3573, 10.1093/mnras/stw224

    2016 doi

  10. [18]

    V., Jord \'a n , A., et al

    Espinoza , N., Rackham , B. V., Jord \'a n , A., et al. 2019, , 482, 2065, 10.1093/mnras/sty2691

    2019 doi

  11. [19]

    M., Aigrain , S., Gibson , N., et al

    Evans , T. M., Aigrain , S., Gibson , N., et al. 2015, , 451, 680, 10.1093/mnras/stv910

    2015 doi

  12. [20]

    M., Sing , D

    Evans , T. M., Sing , D. K., Kataria , T., et al. 2017, , 548, 58, 10.1038/nature23266

    2017 doi

  13. [21]

    M., Sing , D

    Evans , T. M., Sing , D. K., Goyal , J. M., et al. 2018, , 156, 283, 10.3847/1538-3881/aaebff

    2018 doi

  14. [22]

    Faedi , F., Barros , S. C. C., Anderson , D. R., et al. 2011, , 531, A40, 10.1051/0004-6361/201116671

    2011 doi

  15. [23]

    D., Knutson , H

    Fischer , P. D., Knutson , H. A., Sing , D. K., et al. 2016, , 827, 19, 10.3847/0004-637X/827/1/19

    2016 doi

  16. [24]

    2018, , 481, 4698, 10.1093/mnras/sty2550

    Fisher , C., & Heng , K. 2018, , 481, 4698, 10.1093/mnras/sty2550

    2018 doi

  17. [25]

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

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

    2013 doi

  18. [26]

    2017, , 847, L22, 10.3847/2041-8213/aa8e40

    Fu , G., Deming , D., Knutson , H., et al. 2017, , 847, L22, 10.3847/2041-8213/aa8e40

    2017 doi

  19. [27]

    P., Aigrain , S., Roberts , S., et al

    Gibson , N. P., Aigrain , S., Roberts , S., et al. 2012 a , , 419, 2683, 10.1111/j.1365-2966.2011.19915.x

    2012

  20. [28]

    P., Nikolov , N., Sing , D

    Gibson , N. P., Nikolov , N., Sing , D. K., et al. 2017, , 467, 4591, 10.1093/mnras/stx353

    2017 doi

  21. [29]

    P., Aigrain , S., Pont , F., et al

    Gibson , N. P., Aigrain , S., Pont , F., et al. 2012 b , , 422, 753, 10.1111/j.1365-2966.2012.20655.x

    2012

  22. [30]

    M., Mayne , N., Sing , D

    Goyal , J. M., Mayne , N., Sing , D. K., et al. 2018, , 474, 5158, 10.1093/mnras/stx3015

    2018 doi

  23. [31]

    Griffith , C. A. 2014, Philosophical Transactions of the Royal Society of London Series A, 372, 20130086, 10.1098/rsta.2013.0086

    2014

  24. [32]

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

    Haywood , R. D., Collier Cameron , A., Queloz , D., et al. 2014, , 443, 2517, 10.1093/mnras/stu1320

    2014 doi

  25. [33]

    2016, , 826, L16, 10.3847/2041-8205/826/1/L16

    Heng , K. 2016, , 826, L16, 10.3847/2041-8205/826/1/L16

    2016 doi

  26. [34]

    2017, , 470, 2972, 10.1093/mnras/stx1453

    Heng , K., & Kitzmann , D. 2017, , 470, 2972, 10.1093/mnras/stx1453

    2017 doi

  27. [35]

    J., Ehrenreich , D., Heng , K., et al

    Hoeijmakers , H. J., Ehrenreich , D., Heng , K., et al. 2018, , 560, 453, 10.1038/s41586-018-0401-y

    2018 doi

  28. [36]

    J., Ehrenreich , D., Kitzmann , D., et al

    Hoeijmakers , H. J., Ehrenreich , D., Kitzmann , D., et al. 2019, arXiv e-prints, arXiv:1905.02096. 1905.02096

    2019 arXiv

  29. [37]

    Hunter, J. D. 2007, Computing In Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  30. [38]

    2013, , 553, A6, 10.1051/0004-6361/201219058

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

    2013 doi

  31. [39]

    2001, SciPy : Open source scientific tools for Python

    Jones, E., Oliphant, T., Peterson, P., et al. 2001, SciPy : Open source scientific tools for Python . http://www.scipy.org/

    2001

  32. [40]

    M.-R., Lupu , R., Owusu-Asare , A., Slough , P., & Cale , B

    Kempton , E. M.-R., Lupu , R., Owusu-Asare , A., Slough , P., & Cale , B. 2017, , 129, 044402, 10.1088/1538-3873/aa61ef

    2017 doi

  33. [41]

    2018, PhD thesis, University of Warwick

    Kirk , J. 2018, PhD thesis, University of Warwick . https://wrap.warwick.ac.uk/111014/

    2018

  34. [42]

    J., Louden , T., et al

    Kirk , J., Wheatley , P. J., Louden , T., et al. 2017, , 468, 3907, 10.1093/mnras/stx752

    2017 doi

  35. [43]

    2016, , 463, 2922, 10.1093/mnras/stw2205

    ---. 2016, , 463, 2922, 10.1093/mnras/stw2205

    2016 doi

  36. [44]

    2018, , 474, 876, 10.1093/mnras/stx2826

    ---. 2018, , 474, 876, 10.1093/mnras/stx2826

    2018 doi

  37. [45]

    2015, Publications of the Astronomical Society of the Pacific, 127, 1161, 10.1086/683602

    Kreidberg , L. 2015, Publications of the Astronomical Society of the Pacific, 127, 1161, 10.1086/683602

    2015 doi

  38. [46]

    L., D \'e sert , J.-M., et al

    Kreidberg , L., Bean , J. L., D \'e sert , J.-M., et al. 2014, Nature, 505, 69, 10.1038/nature12888

    2014 doi

  39. [47]

    2008, , 481, L83, 10.1051/0004-6361:200809388

    Lecavelier Des Etangs , A., Pont , F., Vidal-Madjar , A., & Sing , D. 2008, , 481, L83, 10.1051/0004-6361:200809388

    2008 doi

  40. [48]

    J., Irwin , P

    Louden , T., Wheatley , P. J., Irwin , P. G. J., Kirk , J., & Skillen , I. 2017, , 470, 742, 10.1093/mnras/stx984

    2017 doi

  41. [49]

    J., & Madhusudhan , N

    MacDonald , R. J., & Madhusudhan , N. 2017, , 469, 1979, 10.1093/mnras/stx804

    2017 doi

  42. [50]

    2012, , 758, 36, 10.1088/0004-637X/758/1/36

    Madhusudhan , N. 2012, , 758, 36, 10.1088/0004-637X/758/1/36

    2012 doi

  43. [51]

    A., & Kennedy , G

    Madhusudhan , N., Amin , M. A., & Kennedy , G. M. 2014, , 794, L12, 10.1088/2041-8205/794/1/L12

    2014 doi

  44. [52]

    2009, , 707, 24, 10.1088/0004-637X/707/1/24

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

    2009 doi

  45. [53]

    2016, , 463, 604

    Mallonn, M., Bernt, I., Herrero, E., et al. 2016, , 463, 604

    2016

  46. [54]

    2018, , 613, A41, 10.1051/0004-6361/201732234

    Mancini , L., Esposito , M., Covino , E., et al. 2018, , 613, A41, 10.1051/0004-6361/201732234

    2018 doi

  47. [55]

    2002, , 580, L171, 10.1086/345520

    Mandel , K., & Agol , E. 2002, , 580, L171, 10.1086/345520

    2002 doi

  48. [56]

    2014, , 791, 55

    McCullough, P., Crouzet, N., Deming, D., & Madhusudhan, N. 2014, , 791, 55

    2014

  49. [57]

    V., Fortney , J

    Morley , C. V., Fortney , J. J., Marley , M. S., et al. 2015, , 815, 110, 10.1088/0004-637X/815/2/110

    2015 doi

  50. [58]

    K., Gibson , N

    Nikolov , N., Sing , D. K., Gibson , N. P., et al. 2016, , 832, 191, 10.3847/0004-637X/832/2/191

    2016 doi

  51. [59]

    K., Fortney , J

    Nikolov , N., Sing , D. K., Fortney , J. J., et al. 2018, , 557, 526, 10.1038/s41586-018-0101-7

    2018 doi

  52. [60]

    I., Murray-Clay , R., & Bergin , E

    \"O berg , K. I., Murray-Clay , R., & Bergin , E. A. 2011, , 743, L16, 10.1088/2041-8205/743/1/L16

    2011 doi

  53. [61]

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

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

    2015 doi

  54. [62]

    2017, ArXiv e-prints

    Parviainen , H., Palle , E., Chen , G., et al. 2017, ArXiv e-prints. 1709.01875

    2017 arXiv

  55. [63]

    2017, , 471, 4355, 10.1093/mnras/stx1849

    Pinhas , A., & Madhusudhan , N. 2017, , 471, 4355, 10.1093/mnras/stx1849

    2017 doi

  56. [64]

    2019, , 482, 1485, 10.1093/mnras/sty2544

    Pinhas , A., Madhusudhan , N., Gandhi , S., & MacDonald , R. 2019, , 482, 1485, 10.1093/mnras/sty2544

    2019 doi

  57. [65]

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

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

    2018 doi

  58. [66]

    L., Moutou , C., & Charbonneau , D

    Pont , F., Knutson , H., Gilliland , R. L., Moutou , C., & Charbonneau , D. 2008, , 385, 109, 10.1111/j.1365-2966.2008.12852.x

    2008

  59. [67]

    K., Gibson , N

    Pont , F., Sing , D. K., Gibson , N. P., et al. 2013, , 432, 2917, 10.1093/mnras/stt651

    2013 doi

  60. [68]

    2017, , 834, 151, 10.3847/1538-4357/aa4f6c

    Rackham , B., Espinoza , N., Apai , D., et al. 2017, , 834, 151, 10.3847/1538-4357/aa4f6c

    2017 doi

  61. [69]

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

    Rackham , B. V., Apai , D., & Giampapa , M. S. 2018, arXiv e-prints, arXiv:1812.06184. 1812.06184

    2018 arXiv

  62. [70]

    A., Reece , S., & Roberts , S

    Rajpaul , V., Aigrain , S., Osborne , M. A., Reece , S., & Roberts , S. 2015, , 452, 2269, 10.1093/mnras/stv1428

    2015 doi

  63. [71]

    P., Venot , O., Lagage , P

    Rocchetto , M., Waldmann , I. P., Venot , O., Lagage , P. O., & Tinetti , G. 2016, , 833, 120, 10.3847/1538-4357/833/1/120

    2016 doi

  64. [72]

    K., Fortney , J

    Sing , D. K., Fortney , J. J., Nikolov , N., et al. 2016, , 529, 59, 10.1038/nature16068

    2016 doi

  65. [73]

    J., Sing , D

    Spake , J. J., Sing , D. K., Evans , T. M., et al. 2018, , 557, 68, 10.1038/s41586-018-0067-5

    2018 doi

  66. [74]

    Stevenson , K. B. 2016, , 817, L16, 10.3847/2041-8205/817/2/L16

    2016 doi

  67. [75]

    Thorngren , D., & Fortney , J. J. 2019, , 874, L31, 10.3847/2041-8213/ab1137

    2019 doi

  68. [76]

    P., Fortney , J

    Thorngren , D. P., Fortney , J. J., Murray-Clay , R. A., & Lopez , E. D. 2016, , 831, 64, 10.3847/0004-637X/831/1/64

    2016 doi

  69. [77]

    P., Zingales , T., et al

    Tsiaras , A., Waldmann , I. P., Zingales , T., et al. 2018, , 155, 156, 10.3847/1538-3881/aaaf75

    2018 doi

  70. [78]

    C., & Varoquaux, G

    Van Der Walt, S., Colbert, S. C., & Varoquaux, G. 2011, Computing in Science & Engineering, 13, 22

    2011

  71. [79]

    R., & Sing , D

    Wakeford , H. R., & Sing , D. K. 2015, , 573, A122, 10.1051/0004-6361/201424207

    2015 doi

  72. [80]

    R., Visscher , C., Lewis , N

    Wakeford , H. R., Visscher , C., Lewis , N. K., et al. 2017, , 464, 4247, 10.1093/mnras/stw2639

    2017 doi

  73. [81]

    R., Sing , D

    Wakeford , H. R., Sing , D. K., Deming , D., et al. 2018, , 155, 29, 10.3847/1538-3881/aa9e4e

    2018 doi

  74. [82]

    2019, , 157, 206, 10.3847/1538-3881/ab14de

    Welbanks , L., & Madhusudhan , N. 2019, , 157, 206, 10.3847/1538-3881/ab14de

    2019 doi

  75. [83]

    S., Freedman , R

    Zahnle , K., Marley , M. S., Freedman , R. S., Lodders , K., & Fortney , J. J. 2009, , 701, L20, 10.1088/0004-637X/701/1/L20

    2009 doi

  76. [84]

    Zhang , M., Chachan , Y., Kempton , E. M. R., & Knutson , H. A. 2019, , 131, 034501, 10.1088/1538-3873/aaf5ad

    2019 doi

  77. [85]

    P., Tollerud, E

    Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al.\ 2013, , 558, A33

    2013

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.