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arxiv: 2606.30112 · v1 · pith:E7W3D5NTnew · submitted 2026-06-29 · 🌌 astro-ph.SR · astro-ph.EP

Asymmetric nightside CO2 features, inefficient heat transport, and precise evolutionary constraints: Spectroscopic phase curves reveal the past and present of a white dwarf-brown dwarf binary

Daphne Broski-Laing , Yifan Zhou , Joshua D. Lothringer , Daniel Apai , Jenni R. French , Sarah L. Casewell , L. C. Mayorga , Lael Shin
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Ben W. P. Lew Xianyu Tan Vivien Parmentier Siyi Xu Mark S. Marley
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Pith reviewed 2026-06-30 04:13 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords white dwarf-brown dwarf binaryJWST phase curveheat transport efficiencyCO2 absorptionsubstellar atmospherescommon envelope evolutionbrown dwarf luminosityatmospheric retrieval
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The pith

Spectroscopic phase curves of a white dwarf-brown dwarf binary show day-to-night heat transport efficiency below 10%.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents the first JWST full-orbit phase curve of the white dwarf-brown dwarf binary ZTFJ0038+2030 observed with NIRSpec PRISM. A total eclipse of the white dwarf allows separation of the two components' emission throughout the orbit, enabling a nearly model-independent energy balance from the spectrum that covers about 80% of the brown dwarf's bolometric output. This yields a day-to-nightside heat transport efficiency below 10%, backed by the nightside spectrum resembling non-irradiated mid-to-late T dwarfs and the overall phase curve shape. The observations also show a strong nightside CO2 absorption asymmetry at 4.2 microns despite longitudinally homogeneous retrieved abundances, and they deliver a precise internal luminosity that constrains the system age to 7.5-8.8 Gyr along with low common-envelope ejection efficiency. A sympathetic reader would care because the results directly connect tidally locked brown dwarf atmospheres to hot Jupiter dynamics and supply new constraints on post-main-sequence planetary system evolution.

Core claim

The spectroscopic phase curves reveal inefficient heat redistribution with day-to-nightside heat transport efficiency below 10%, derived from a nearly model-independent energy balance calculation using the PRISM spectrum covering ~80% of the brown dwarf's bolometric emission. Inefficient redistribution is further supported by the phase curve shape and the nightside spectrum closely resembling non-irradiated mid-to-late T dwarfs. The data show a stark nightside asymmetry tied to strong CO2 absorption at 4.2 um, while retrieved abundances indicate longitudinally homogeneous distributions of CO2 and other key species. The precise internal luminosity measurement informs both the age of the WD-BD

What carries the argument

The NIRSpec PRISM full-orbit phase curve including total white dwarf eclipse, which separates the brown dwarf's phase-resolved emission spectra for energy balance and retrieval analysis.

If this is right

  • Tidally locked brown dwarfs in short-period binaries exhibit hot Jupiter-like atmospheric dynamics with very inefficient day-to-night heat redistribution.
  • Nightside CO2 absorption features and asymmetries serve as probes of three-dimensional processes in substellar atmospheres.
  • Precise brown dwarf luminosity measurements tightly constrain system ages and common-envelope ejection efficiencies in post-main-sequence binaries.
  • WD-BD binaries act as laboratories connecting substellar atmospheres to exoplanet atmospheres and probing planetary system evolution after the host star leaves the main sequence.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Additional WD-BD systems observed with similar full-orbit spectroscopy could test whether sub-10% heat transport efficiency is typical for tidally locked brown dwarf companions.
  • The combination of nightside asymmetry with homogeneous abundances may indicate chemical or dynamical mechanisms that current forward models do not fully capture.
  • The technique of using eclipses for component separation could extend to other irradiated substellar companions to map heat transport across a range of irradiation levels.

Load-bearing premise

The NIRSpec PRISM spectrum and eclipse geometry allow clean separation of the white dwarf and brown dwarf emission components throughout the orbit without significant contamination or model-dependent corrections.

What would settle it

A nightside spectrum measured independently at wavelengths where the white dwarf contribution is negligible that deviates substantially from a non-irradiated mid-to-late T dwarf spectrum, or an energy balance yielding heat transport efficiency well above 10%, would falsify the inefficient transport claim.

Figures

Figures reproduced from arXiv: 2606.30112 by Ben W. P. Lew, Daniel Apai, Daphne Broski-Laing, Jenni R. French, Joshua D. Lothringer, Lael Shin, L. C. Mayorga, Mark S. Marley, Sarah L. Casewell, Siyi Xu, Vivien Parmentier, Xianyu Tan, Yifan Zhou.

Figure 1
Figure 1. Figure 1: Left: Outline of the custom spectral extraction pipeline used to generate absolute flux-calibrated time-series spectra. Right: intermediate data products generated at various stages throughout the reduction process: (A) relative flux-calibrated spectral time series produced by Eureka!; (B) flux-calibrated and exposure-averaged spectra produced by the jwst pipeline; (C) master calibration factor array; and … view at source ↗
Figure 2
Figure 2. Figure 2: Absolute flux-calibrated spectra of the combined white dwarf–brown dwarf signal. As the brown dwarf eclipses the white dwarf, the flux decreases dramatically in the shorter wavelengths where the white dwarf signal dominates. The outlier integrations are shown in dashed green lines. σν,med spec = sν,combined/ p Ncombined ints − 1 (5) Next, we select a subset of out-of-eclipse integrations which contain the … view at source ↗
Figure 3
Figure 3. Figure 3: Overview of the procedure to separate the white dwarf and brown dwarf emission signals. The upper-left panel shows the broadband flux around the time of the eclipse. During the total eclipse (purple), we observe the brown dwarf’s nightside emission without white dwarf contamination. Frames immediately before and after the eclipse (pink) contain combined signals from both objects. Subtracting the isolated n… view at source ↗
Figure 4
Figure 4. Figure 4: The broadband phase curve and a selection of 10 spectroscopic phase curves were produced for ZTF0038B (every 5 of the 50 evenly-spaced wavelength bins). Each phase curve is fit with a second order Fourier series with the period found with the eclipse timing analysis ( [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Best-fit batman transit model of ZTF0038 fit via MCMC using emcee. The brown dwarf’s emission is subtracted, and flux is normalized such that the out-of-eclipse signal is centered around one, and the flux goes to zero during the total eclipse. The propagated ephemeris is t0, propagated = 60648.34328 ± 8.5 × 10−5MJDTDB. The period and ephemeris from our eclipse timing analysis agree with this prediction to … view at source ↗
Figure 6
Figure 6. Figure 6: Several multi-component sinusoidal model fits of the broadband phase curve of ZTF0038B. The top row uses a single sinusoid to fit the data, and each row below adds an additional term. The first column fits the model assuming the period found in our eclipse timing analysis ( [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Fourier amplitudes and phases of the spectroscopic phase curves as a function of wavelength. Each phase curve is fit with a second-order Fourier series; bins consistent with a flat model are indicated with black squares. In each panel, we include the phase curve information for 50 evenly spaced wavelength bins as well as a few additional wavelength bins corresponding to H2O, CH4, CO2, and CO absorption fea… view at source ↗
Figure 8
Figure 8. Figure 8: Illustration of the WD–BD geometry at eight representative phases in the orbit. The upper illustrations visualize a simple representation of the brown dwarf hemisphere observed at each phase. The shading indicates how much of the dayside (pink) and nightside hemisphere (purple) are visible at each phase. In phases A and E (nightside and dayside), the smaller central circle indicates when the white dwarf is… view at source ↗
Figure 9
Figure 9. Figure 9: Emission spectra of ZTF0038B at 8 representative phases (top panel) and their associated signal-to-noise ratios (bottom panel) [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the observed ZTF0038B spectrum (black) with archival JWST PRISM spectra of mid-to-late T dwarfs (S. A. Beiler et al. 2024). We uniformly scale the archival spectra to minimize the chi-squared statistic across the entire wavelength range (left) and across the J, H, and K bands only (right). We verified that a cloud-free model was preferred by comparing the Elf Owl fit with the Sonora Diamond￾… view at source ↗
Figure 11
Figure 11. Figure 11: Top: ZTF0038B day and nightside brightness temperature. Bottom: Difference between the dayside and nightside brightness temperatures. parameters limited to discrete grid points, and therefore do not include uncertainties. 4.5. Joint, Chemically-Constrained Retrieval We performed atmospheric retrievals using the petitRadTrans radiative transfer framework (P. Molli`ere et al. 2019). The retrieval employs ne… view at source ↗
Figure 12
Figure 12. Figure 12: Nightside (left) and dayside (right) spectra of ZTF0038B compared with the best-fitting models obtained using forward-modeling grids and atmospheric retrievals. The joint retrieval successfully reproduced the ob￾served spectra across all phases, except in the λ > 4 µm region, where CO2 absorption shapes the spec￾trum. The retrieval also struggles to fit CO2 even if the phases are fit independently. Global… view at source ↗
Figure 13
Figure 13. Figure 13: Joint multi-phase spectroscopic retrieval results. Upper panel: the retrieved temperature profiles for all eight phases. Lower panels: the observed and retrieved spectra for eight representative phases, as well as the residuals [PITH_FULL_IMAGE:figures/full_fig_p019_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: We use the brightness temperatures presented in Section 4.3 and the TP profiles from our joint retrieval to map the brightness temperature to its associated photospheric pressure value at each wavelength. 0.0 0.2 0.4 0.6 0.8 Orbital Phase 6 5 4 3 2 Log (Mass Fraction) CO H O CO CH NH 0.0 0.2 0.4 0.6 0.8 Orbital Phase 12 10 8 6 4 2 0 Log (Mass Fraction) HCN H S PH Na K FeH Molecular Abundances From Free Re… view at source ↗
Figure 15
Figure 15. Figure 15: Retrieved abundances for 11 species as a function of phase, as determined via free retrievals for each of the eight phases. Dashed lines indicate the median abundances for each species. For a tidally locked atmosphere with inefficient heat transport, the expected temperature structure would yield a symmetric light curve with a minimum during the mid-eclipse time (phase =0) and a maximum at the substellar … view at source ↗
Figure 16
Figure 16. Figure 16: An overview of the observational detections of an asymmetric CO2 absorption feature. The top left panel shows the phase resolved absorption spectra from 1.6 - 5.3 µm with highlighted regions corresponding to molecular absorption features and continuum regions. The phase curves for these regions are plotted in the upper right panel. Each phase curve is shown with the best-fitting phase curve model (as disc… view at source ↗
Figure 17
Figure 17. Figure 17: Constraints on bond albedo, redistributed flux fraction, and internal luminosity from energy balance equations. In both panels, three calculations are shown using a range of plausible bolometric corrections (fbol). The maximum and minimum fbol represent the nominal uncertainty range for the central, fiducial calculation. Top: Day-night redistribution efficiency represents the fraction of the irradiation e… view at source ↗
Figure 18
Figure 18. Figure 18: Comparison of the retrieved abundances and predictions from chemical equilibrium. H2O (blue), CH4 (pink), CO (yellow), and CO2 (fuchsia) abundances are shown from the free retrieval (circles), joint retrievals (triangles), and the chemical equilibrium prediction (squares). H2O and CH4 are both consistent with the chemical equilibrium predictions, while the retrieved abundances for both CO and CO2 are larg… view at source ↗
Figure 19
Figure 19. Figure 19: Luminosity constraints from the energy balance calculation for ZTF0038B (horizontal lines) are compared with field brown dwarf evolutionary tracks (solid blue and green curves). The shaded regions around the evolutionary tracks indicate the uncertainty in the evolutionary models based on the mass uncertainty from J. van Roestel et al. (2021). The horizontal dashed lines indicate age constraints from this … view at source ↗
Figure 20
Figure 20. Figure 20: Corner plot of the MCMC eclipse fitting using a batman transit model. The best-fit model is shown in [PITH_FULL_IMAGE:figures/full_fig_p032_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Corner plot showing the posterior distributions from nested sampling of the Sonora Elf Owl grid fit to the brown dwarf’s nightside spectrum (S. Mukherjee et al. 2024). We use normal priors for log(g), Rp, ω, and M, as shown blue dashed lines in the relevant parameter histograms [PITH_FULL_IMAGE:figures/full_fig_p034_21.png] view at source ↗
read the original abstract

We present the first JWST phase curve of a white dwarf-brown dwarf binary, a NIRSpec PRISM observation of ZTFJ0038+2030. Short-period white dwarf-brown dwarf binaries provide unique laboratories to probe substellar atmospheres. Tidal locking drives hot Jupiter-like atmospheric dynamics in the brown dwarf. The system's formation history offers a window into planetary systems around post-main-sequence stars. We obtain a full-orbit phase curve of ZTF0038, including a total eclipse of the white dwarf, which enables us to separate the two components' emission throughout the entire orbit, and we model the brown dwarf's phase-resolved emission spectra using substellar atmosphere forward models and atmospheric retrievals. The PRISM spectrum covers ~80% of the brown dwarf's bolometric emission, enabling a nearly model-independent energy balance calculation, which yields a day-to-nightside heat transport efficiency of <10%. Inefficient heat redistribution is further supported by the phase curve shape and the nightside spectrum closely resembling non-irradiated mid-to-late T dwarfs. The spectroscopic phase curves reveal a stark nightside asymmetry associated with a strong CO2 absorption feature at 4.2 um, while the retrieved abundances indicate a longitudinally homogeneous distribution of CO2 as well as all other key species detected in the atmosphere. The precise internal luminosity measurement of the brown dwarf informs both the age of the WD-BD system (7.5-8.8 Gyr) and indicates a low common-envelope ejection efficiency. These data illustrate the exquisite opportunity to probe the three-dimensional processes of substellar atmospheres, connect substellar and exoplanet atmospheres, and probe the evolution of post-main-sequence planetary systems using WD-BDs.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript reports the first JWST NIRSpec PRISM spectroscopic phase curve of the white dwarf-brown dwarf binary ZTF J0038+2030. Leveraging a total eclipse to separate the white dwarf and brown dwarf emission components throughout the orbit, the authors apply substellar atmosphere forward models and retrievals to the phase-resolved brown dwarf spectra. They perform a nearly model-independent energy balance calculation over the ~80% bolometric coverage of the PRISM spectrum to derive a day-to-nightside heat transport efficiency of <10%, corroborated by the phase curve shape and nightside spectrum resembling non-irradiated mid-to-late T dwarfs. Additional findings include a nightside asymmetry linked to a strong CO2 absorption feature at 4.2 μm (with longitudinally homogeneous retrieved abundances for CO2 and other species) and a precise internal luminosity that constrains the system age to 7.5-8.8 Gyr and implies low common-envelope ejection efficiency.

Significance. If the component separation and energy balance hold, the result supplies a rare, direct constraint on inefficient heat redistribution in a tidally locked substellar atmosphere, with clear connections to hot Jupiter dynamics and the evolution of post-main-sequence planetary systems. The broad spectral coverage enabling a nearly model-independent efficiency calculation is a methodological strength.

major comments (2)
  1. [Abstract] Abstract and energy-balance section: The <10% day-to-nightside heat transport efficiency is derived from integrated day- and nightside fluxes after subtracting a constant white dwarf contribution measured from the total eclipse depth. The manuscript must supply quantitative tests (e.g., wavelength-dependent eclipse depth residuals, checks for brown dwarf variability on the eclipse timescale, and PRISM systematic differences between in- and out-of-eclipse data) to demonstrate that residual contamination does not bias the nightside flux at a level that would alter the efficiency upper limit.
  2. [Abstract] The assumption that the NIRSpec PRISM spectrum and eclipse geometry permit clean separation of the two components without model-dependent corrections is load-bearing for both the efficiency claim and the nightside asymmetry interpretation; any non-constant white dwarf flux or incomplete totality at 4.2 μm would propagate directly into the reported CO2 feature and energy balance.
minor comments (1)
  1. Clarify in the methods whether the 80% bolometric coverage fraction is calculated from the observed spectrum alone or incorporates any model extrapolation, and state the precise wavelength range used for the integration.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and for highlighting the importance of rigorously validating the component separation. We address the major comments below and will revise the manuscript to incorporate the requested quantitative tests.

read point-by-point responses

  1. Referee: [Abstract] Abstract and energy-balance section: The <10% day-to-nightside heat transport efficiency is derived from integrated day- and nightside fluxes after subtracting a constant white dwarf contribution measured from the total eclipse depth. The manuscript must supply quantitative tests (e.g., wavelength-dependent eclipse depth residuals, checks for brown dwarf variability on the eclipse timescale, and PRISM systematic differences between in- and out-of-eclipse data) to demonstrate that residual contamination does not bias the nightside flux at a level that would alter the efficiency upper limit.

    Authors: We agree that explicit quantitative validation of the constant white dwarf subtraction is essential to support the efficiency upper limit. In the revised manuscript we will add: (1) wavelength-dependent eclipse depth residuals across the PRISM range, (2) an assessment of brown dwarf variability on the eclipse timescale using the out-of-eclipse baseline, and (3) a direct comparison of PRISM systematic trends inside versus outside eclipse. These tests will quantify any residual contamination and confirm it does not alter the reported <10% day-to-nightside heat transport efficiency. revision: yes

  2. Referee: [Abstract] The assumption that the NIRSpec PRISM spectrum and eclipse geometry permit clean separation of the two components without model-dependent corrections is load-bearing for both the efficiency claim and the nightside asymmetry interpretation; any non-constant white dwarf flux or incomplete totality at 4.2 μm would propagate directly into the reported CO2 feature and energy balance.

    Authors: The observation is of a total eclipse, which in principle enables direct, model-independent separation of the components. To address the referee's concern about possible non-constant white dwarf flux or wavelength-dependent incompleteness (particularly near 4.2 μm), the revision will include an explicit verification of eclipse totality across the full PRISM bandpass, including at the CO2 feature, together with any constraints on white dwarf variability. These additions will strengthen the justification for the clean separation used in both the energy-balance and nightside asymmetry analyses. revision: yes

Circularity Check

0 steps flagged

No circularity: heat transport efficiency derived directly from observed spectra and eclipse geometry

full rationale

The central result (day-to-nightside heat transport efficiency <10%) is obtained by integrating the PRISM spectra (~80% bolometric coverage) after separating WD and BD components via the total eclipse, then comparing emitted power on each side to the irradiation inferred from the WD eclipse depth. This is a direct observational energy balance with no equations reducing the output to a fitted input renamed as prediction, no self-definitional loop, and no load-bearing self-citation chain. The separation relies on eclipse geometry rather than an ansatz or prior result from the same authors. The derivation is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The efficiency bound rests on the claim that the PRISM spectrum captures ~80% of bolometric flux (an observational coverage assumption) and on the accuracy of substellar atmosphere forward models used for retrievals. No new particles or forces are introduced. The age constraint depends on internal luminosity models whose free parameters (e.g., metallicity, cloud properties) are not enumerated in the abstract.

free parameters (2)
  • day-to-night heat transport efficiency
    Derived from energy balance; treated as a fitted or bounded quantity rather than predicted from first principles.
  • atmospheric retrieval parameters (abundances, temperature profile)
    Standard retrieval parameters whose values are adjusted to match the observed spectra.
axioms (2)
  • domain assumption Tidal locking produces hot-Jupiter-like atmospheric dynamics in the brown dwarf
    Invoked to justify the dynamical regime but not derived in the abstract.
  • domain assumption Substellar atmosphere forward models accurately represent the emission spectra
    Required for both the phase-curve modeling and the retrievals.

pith-pipeline@v0.9.1-grok · 5917 in / 1597 out tokens · 30466 ms · 2026-06-30T04:13:06.286439+00:00 · methodology

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Reference graph

Works this paper leans on

117 extracted references · 47 canonical work pages · 9 internal anchors

  1. [1]

    Exoplanet Reflected Light Spectroscopy with PICASO

    doi:10.3847/1538-4357/ab1b51 , eid =. arXiv , author =:1904.09355 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1b51 1904

  2. [2]

    arXiv , author =:2110.10158 , journal =

    doi:10.3847/1538-3881/ac3001 , eid =. arXiv , author =:2110.10158 , journal =

    work page doi:10.3847/1538-3881/ac3001

  3. [3]

    doi:10.1086/321540 , eprint =

    , keywords =. doi:10.1086/321540 , eprint =

    work page doi:10.1086/321540

  4. [4]

    arXiv , author =:2303.07420 , journal =

    doi:10.3847/1538-4357/acbfb3 , eid =. arXiv , author =:2303.07420 , journal =

    work page doi:10.3847/1538-4357/acbfb3

  5. [5]

    doi:10.1093/mnras/stae2121 , eprint =

    , keywords =. doi:10.1093/mnras/stae2121 , eprint =

    work page doi:10.1093/mnras/stae2121

  6. [6]

    doi:10.1086/306881 , eprint =

    , keywords =. doi:10.1086/306881 , eprint =

    work page doi:10.1086/306881

  7. [7]

    Handbook of Exoplanets , doi =

  8. [8]

    arXiv , author =:2006.09394 , journal =

    doi:10.1051/0004-6361/202038325 , eid =. arXiv , author =:2006.09394 , journal =

    work page doi:10.1051/0004-6361/202038325 2006

  9. [9]

    ascl , author =:1905.019 , howpublished =

    1905

  10. [10]

    arXiv , author =:2105.08009 , journal =

    doi:10.3847/1538-4357/abff50 , eid =. arXiv , author =:2105.08009 , journal =

    work page doi:10.3847/1538-4357/abff50

  11. [11]

    arXiv , author =:2107.07434 , journal =

    doi:10.3847/1538-4357/ac141d , eid =. arXiv , author =:2107.07434 , journal =

    work page doi:10.3847/1538-4357/ac141d

  12. [12]

    arXiv , author =:2402.00756 , journal =

    doi:10.3847/1538-4357/ad18c2 , eid =. arXiv , author =:2402.00756 , journal =

    work page doi:10.3847/1538-4357/ad18c2

  13. [13]

    arXiv , author =:2404.16813 , journal =

    doi:10.3847/1538-4357/ad43da , eid =. arXiv , author =:2404.16813 , journal =

    work page doi:10.3847/1538-4357/ad43da

  14. [14]

    petitRADTRANS: a Python radiative transfer package for exoplanet characterization and retrieval

    doi:10.1051/0004-6361/201935470 , eid =. arXiv , author =:1904.11504 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935470 1904

  15. [15]

    American Institute of Physics Conference Series , doi =

  16. [16]

    A., Beardmore, A

    , keywords =. doi:10.1111/j.1365-2966.2009.14548.x , eprint =

    work page doi:10.1111/j.1365-2966.2009.14548.x 2009

  17. [17]

    doi:10.1086/683602 , eprint =

    , keywords =. doi:10.1086/683602 , eprint =

    work page internal anchor Pith review doi:10.1086/683602

  18. [18]

    and Radica, Michael and Welbanks, Luis and Murray, Catriona A

    Feinstein, Adina D. and Radica, Michael and Welbanks, Luis and Murray, Catriona A. and Ohno, Kazumasa and Coulombe, Louis P. and Espinoza, N. Early Release Science of the exoplanet. doi:10.1038/s41586-022-05674-1 , journal =

    work page doi:10.1038/s41586-022-05674-1

  19. [19]

    Carter, A. L. and May, E. M. and Espinoza, N. A benchmark. doi:10.1038/s41550-024-02292-x , journal =

    work page doi:10.1038/s41550-024-02292-x

  20. [20]

    JWST Calibration Pipeline , year =

    Bushouse, Howard and Eisenhamer, Jonathan and Dencheva, Nadia and Davies, James and Greenfield, Perry and Morrison, Jane and Hodge, Phil and Simon, Bernie and Grumm, David and Droettboom, Michael and Slavich, Edward and Sosey, Megan and Pauly, Tyler and Miller, Todd and Jedrzejewski, Robert and Hack, Warren and Davis, David and Crawford, Steven and Law, D...

  21. [21]

    and Ahrer, Eva-Maria and Brande, Jonathan and Carter, Aarynn L

    Bell, Taylor J. and Ahrer, Eva-Maria and Brande, Jonathan and Carter, Aarynn L. and Feinstein, Adina D. and Guzman Caloca, Giannina and Mansfield, Megan and Zieba, Sebastian and Piaulet, Caroline and Benneke, Björn and Filippazzo, Joseph and May, Erin M. and Roy, Pierre-Alexis and Kreidberg, Laura and Stevenson, Kevin B. , doi =. Journal of Open Source So...

  22. [22]

    doi:10.1038/nature04987 , journal =

    Discovery of a brown dwarf companion to the white dwarf WD 0137-349 , volume =. doi:10.1038/nature04987 , journal =

    work page doi:10.1038/nature04987

  23. [23]

    , keywords =

    A post-common-envelope binary with a brown dwarf companion: WD 0137-349 , volume =. doi:10.1111/j.1745-3933.2006.00248.x , journal =

    work page doi:10.1111/j.1745-3933.2006.00248.x 2006

  24. [24]

    doi:10.3847/1538-4357/aa855f , journal =

    The Origin of White Dwarf–Brown Dwarf Binaries: CE Evolution, Survival Limits, and Formation Channels , volume =. doi:10.3847/1538-4357/aa855f , journal =

    work page doi:10.3847/1538-4357/aa855f

  25. [25]

    Close detached white dwarf + brown dwarf binaries: further evidence for low values of the common envelope efficiency , volume =

    Zorotovic, Monica and Schreiber, MatthiasR , doi =. Close detached white dwarf + brown dwarf binaries: further evidence for low values of the common envelope efficiency , volume =. , keywords =

  26. [26]

    doi:10.1093/mnras/stu2660 , journal =

    Orbital phase–dependent irradiation of the brown dwarf companion WD 0137-349B , volume =. doi:10.1093/mnras/stu2660 , journal =

    work page doi:10.1093/mnras/stu2660

  27. [27]

    doi:10.3847/1538-4357/abb3d4 , eid =

    , pages =. doi:10.3847/1538-4357/abb3d4 , eid =

    work page doi:10.3847/1538-4357/abb3d4

  28. [28]

    doi:10.1093/mnras/staa1882 , eprint =

    , keywords =. doi:10.1093/mnras/staa1882 , eprint =

    work page doi:10.1093/mnras/staa1882

  29. [29]

    arXiv , author =:2010.14319 , journal =

    doi:10.3847/1538-4357/abc5bc , eid =. arXiv , author =:2010.14319 , journal =

    work page doi:10.3847/1538-4357/abc5bc 2010

  30. [30]

    arXiv , author =:2007.15363 , journal =

    doi:10.1007/s11214-020-00758-8 , eid =. arXiv , author =:2007.15363 , journal =

    work page doi:10.1007/s11214-020-00758-8 2007

  31. [31]

    doi:10.1038/nature05782 , eprint =

    , keywords =. doi:10.1038/nature05782 , eprint =

    work page doi:10.1038/nature05782

  32. [32]

    doi:10.1126/science.1256758 , eprint =

    Science , keywords =. doi:10.1126/science.1256758 , eprint =

    work page doi:10.1126/science.1256758

  33. [33]

    arXiv , author =:2501.05609 , journal =

    doi:10.3847/1538-4357/ada295 , eid =. arXiv , author =:2501.05609 , journal =

    work page doi:10.3847/1538-4357/ada295

  34. [34]

    and Lang, Dustin and Goodman, Jonathan , doi =

    Foreman-Mackey, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan , doi =. emcee:. , keywords =

  35. [35]

    Exoplanetary

    Madhusudhan, Nikku , doi =. Exoplanetary. , keywords =

  36. [36]

    and Line, Michael R

    Greene, Thomas P. and Line, Michael R. and Montero, Cezar and Fortney, Jonathan J. and Lustig-Yaeger, Jacob and Luther, Kyle , doi =. Characterizing. , keywords =

  37. [37]

    Atmospheric

    Madhusudhan, Nikku , doi =. Atmospheric

  38. [38]

    and Rojo, P

    Lira-Barria, A. and Rojo, P. M. and Mendez, R. A. , doi =. Characterization of exoplanetary atmospheres through a model-unbiased spectral survey methodology , volume =. Astronomy & Astrophysics , month =

  39. [39]

    and Lew, Ben W

    Zhou, Yifan and Apai, Dániel and Tan, Xianyu and Lothringer, Joshua D. and Lew, Ben W. P. and Casewell, Sarah L. and Parmentier, Vivien and Marley, Mark S. and Xu, Siyi and Mayorga, L. C. , doi =. , keywords =

  40. [40]

    and Singh, H

    Deb, S. and Singh, H. P. , doi =. Light curve analysis of variable stars using. Astronomy & Astrophysics , month =

  41. [41]

    Katherina and Line, Michael R

    Feng, Y. Katherina and Line, Michael R. and Fortney, Jonathan J. , doi =. , keywords =

  42. [42]

    and Riedel, Adric R

    Faherty, Jacqueline K. and Riedel, Adric R. and Cruz, Kelle L. and Gagne, Jonathan and Filippazzo, Joseph C. and Lambrides, Erini and Fica, Haley and Weinberger, Alycia and Thorstensen, John R. and Tinney, C. G. and Baldassare, Vivienne and Lemonier, Emily and Rice, Emily L. , doi =. Population. , keywords =

  43. [43]

    and Dong, Jiayin and Foreman-Mackey, Daniel and Kataria, Tiffany and Barstow, Joanna K

    Mikal-Evans, Thomas and Sing, David K. and Dong, Jiayin and Foreman-Mackey, Daniel and Kataria, Tiffany and Barstow, Joanna K. and Goyal, Jayesh M. and Lewis, Nikole K. and Lothringer, Joshua D. and Mayne, Nathan J. and Wakeford, Hannah R. and Christie, Duncan A. and Rustamkulov, Zafar , doi =. A. , keywords =

  44. [44]

    Signs of accretion in the white dwarf + brown dwarf binary

    Longstaff, E S and Casewell, S L and Wynn, G A and Page, K L and Williams, P K G and Braker, I and Maxted, P F L , doi =. Signs of accretion in the white dwarf + brown dwarf binary. , month =

  45. [45]

    and Bildsten, Lars and Cantiello, Matteo and Lai, Dong , doi =

    O'Connor, Christopher E. and Bildsten, Lars and Cantiello, Matteo and Lai, Dong , doi =. Giant. , keywords =

  46. [46]

    Perets, Hagai B. , doi =. Second generation planets , year =

  47. [47]

    and Naoz, Smadar and Gaudi, B

    Stephan, Alexander P. and Naoz, Smadar and Gaudi, B. Scott , doi =. Giant. , keywords =

  48. [48]

    , month =

    Casewell, S L and Debes, J and Braker, I P and Cushing, M C and Mace, G and Marley, M S and Kirkpatrick, J Davy , doi =. , month =

  49. [49]

    and Cushing, Michael C

    Beiler, Samuel A. and Cushing, Michael C. and Kirkpatrick, J. Davy and Schneider, Adam C. and Mukherjee, Sagnick and Marley, Mark S. and Marocco, Federico and Smart, Richard L. , doi =. Precise

  50. [50]

    and Cushing, Michael C

    Beiler, Samuel A. and Cushing, Michael C. and Kirkpatrick, J. Davy and Schneider, Adam C. and Mukherjee, Sagnick and Marley, Mark S. and Marocco, Federico and Smart, Richard L. , doi =. Precise. , keywords =

  51. [51]

    and Burdge, Kevin and Mróz, Przemek and Prince, Thomas A

    van Roestel, Jan and Kupfer, Thomas and Bell, Keaton J. and Burdge, Kevin and Mróz, Przemek and Prince, Thomas A. and Bellm, Eric C. and Drake, Andrew and Dekany, Richard and Mahabal, Ashish A. and Porter, Michael and Riddle, Reed and Shin, Kyung Min and Shupe, David L. and Kulkarni, S. R. , doi =. , keywords =

  52. [52]

    Exoplanet

    Seager, Sara and Deming, Drake , doi =. Exoplanet. , keywords =

  53. [53]

    and Amundsen, D

    Tremblin, P. and Amundsen, D. S. and Chabrier, G. and Baraffe, I. and Drummond, B. and Hinkley, S. and Mourier, P. and Venot, O. , doi =. Cloudless. , keywords =

  54. [54]

    and Bézard, B

    Charnay, B. and Bézard, B. and Baudino, J. -L. and Bonnefoy, M. and Boccaletti, A. and Galicher, R. , doi =. A. , keywords =

  55. [55]

    Evolutionary models of cold and low-mass planets: cooling curves, magnitudes, and detectability -

  56. [56]

    and Vos, Johanna M

    McCarthy, Allison M. and Vos, Johanna M. and Muirhead, Philip S. and Biller, Beth A. and Morley, Caroline V. and Faherty, Jacqueline and Burningham, Ben and Calamari, Emily and Cowan, Nicolas B. and Cruz, Kelle L. and Gonzales, Eileen and Limbach, Mary Anne and Liu, Pengyu and Nasedkin, Evert and Suarez, Genaro and Tan, Xianyu and O'Toole, Cian and Vissch...

  57. [57]

    and Muirhead, Philip S

    McCarthy, Allison M. and Muirhead, Philip S. and Tamburo, Patrick and Vos, Johanna M. and Morley, Caroline V. and Faherty, Jacqueline and Bardalez Gagliuffi, Daniella C. and Agol, Eric and Theissen, Christopher , doi =. Multiple. , keywords =

  58. [58]

    Madhusudhan, Nikku , doi =. C/. , keywords =

  59. [59]

    Yang, Jingxuan and Hammond, Mark and Piette, Anjali A. A. and Blecic, Jasmina and Bell, Taylor J. and Irwin, Patrick G. J. and Parmentier, Vivien and Tsai, Shang-Min and Barstow, Joanna K. and Crouzet, Nicolas and Kreidberg, Laura and Mendonça, João M. and Taylor, Jake and Baeyens, Robin and Ohno, Kazumasa and Teinturier, Lucas and Nixon, Matthew C. , doi...

  60. [60]

    and Barman, Travis and Koskinen, Tommi , doi =

    Lothringer, Joshua D. and Barman, Travis and Koskinen, Tommi , doi =. Extremely. , keywords =

  61. [61]

    and Mayorga, L

    Jacobs, Bob and Désert, Jean-Michel and Lewis, Nikole and Challener, Ryan C. and Mayorga, L. C. and de Beurs, Zoë L. and Parmentier, Vivien and Stevenson, Kevin B. and de Wit, Julien and Barat, Saugata and Fortney, Jonathan and Kataria, Tiffany and Line, Michael , doi =. Spectroscopically. , keywords =

  62. [62]

    MacDonald, Ryan J. , doi =. The Journal of Open Source Software , keywords =

  63. [63]

    and Gillon, M

    de Wit, J. and Gillon, M. and Demory, B. -O. and Seager, S. , doi =. Towards consistent mapping of distant worlds: secondary-eclipse scanning of the exoplanet. , keywords =

  64. [64]

    Majeau, Carl and Agol, Eric and Cowan, Nicolas B. , doi =. A. , keywords =

  65. [65]

    Mullens, Elijah and Challener, Ryan and Boehm, Victoria Abigail and Crossfield, Ian and Faherty, Jacqueline Kelly and Gonzales, Eileen and Huckabee, Isabela Grace and Kataria, Tiffany and Lacy, Brianna Irene and Lally, Maura and Lewis, Nikole and Suarez, Genaro and Visscher, Channon and Vos, Johanna , journal =. Brown

  66. [66]

    and Lewis, Nikole K

    Lally, Maura and Challener, Ryan C. and Lewis, Nikole K. and Inglis, Julie and Kataria, Tiffany and Knutson, Heather A. and Kilpatrick, Brian M. and Batalha, Natasha E. and Bonney, Paul and Crossfield, Ian J. M. and Foote, Trevor and Henry, Gregory W. and Sing, David K. and Stevenson, Kevin B. and Wakeford, Hannah R. and Zellem, Robert T. , doi =. Eclipse...

  67. [67]

    and Schwartz, Joel C

    Dang, Lisa and Cowan, Nicolas B. and Schwartz, Joel C. and Rauscher, Emily and Zhang, Michael and Knutson, Heather A. and Line, Michael and Dobbs-Dixon, Ian and Deming, Drake and Sundararajan, Sudarsan and Fortney, Jonathan J. and Zhao, Ming , doi =. Detection of a westward hotspot offset in the atmosphere of hot gas giant. Nature Astronomy , keywords =

  68. [68]

    and Aly, Hossam and Winter, Andrew and Longarini, Cristiano and Cuello, Nicolás and Veras, Dimitri and Alexander, Richard , doi =

    Nealon, Rebecca and Smallwood, Jeremy L. and Aly, Hossam and Winter, Andrew and Longarini, Cristiano and Cuello, Nicolás and Veras, Dimitri and Alexander, Richard , doi =. Disc-planet misalignment from an unstable triple system:

  69. [69]

    Taylor, Jake and Parmentier, Vivien and Irwin, Patrick G. J. and Aigrain, Suzanne and Lee, Elspeth K. H. and Krissansen-Totton, Joshua , doi =. Understanding and mitigating biases when studying inhomogeneous emission spectra with. , keywords =

  70. [70]

    Parsons, S. G. and Brown, A. J. and Casewell, S. L. and Littlefair, S. P. and van Roestel, J. and Rebassa-Mansergas, A. and Murillo-Ojeda, R. and Hollands, M. A. and Zorotovic, M. and Castro Segura, N. and Dhillon, V. S. and Dyer, M. J. and Garbutt, J. A. and Green, M. J. and Jarvis, D. and Kennedy, M. R. and Kerry, P. and McCormac, J. and Munday, J. and ...

  71. [71]

    and Crouzet, Nicolas and Cubillos, Patricio E

    Bell, Taylor J. and Crouzet, Nicolas and Cubillos, Patricio E. and Kreidberg, Laura and Piette, Anjali A. A. and Roman, Michael T. and Barstow, Joanna K. and Blecic, Jasmina and Carone, Ludmila and Coulombe, Louis-Philippe and Ducrot, Elsa and Hammond, Mark and Mendonça, João M. and Moses, Julianne I. and Parmentier, Vivien and Stevenson, Kevin B. and Tei...

  72. [72]

    and Biller, Beth A

    Miles, Brittany E. and Biller, Beth A. and Patapis, Polychronis and Worthen, Kadin and Rickman, Emily and Hoch, Kielan K. W. and Skemer, Andrew and Perrin, Marshall D. and Whiteford, Niall and Chen, Christine H. and Sargent, B. and Mukherjee, Sagnick and Morley, Caroline V. and Moran, Sarah E. and Bonnefoy, Mickael and Petrus, Simon and Carter, Aarynn L. ...

  73. [73]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. doi:10.1038/s41592-019-0686-2 , journal =

    work page doi:10.1038/s41592-019-0686-2

  74. [74]

    Zenodo , month =

    Bushouse, Howard and Eisenhamer, Jonathan and Dencheva, Nadia and Davies, James and Greenfield, Perry and Morrison, Jane and Hodge, Phil and Simon, Bernie and Grumm, David and Droettboom, Michael and Slavich, Edward and Sosey, Megan and Pauly, Tyler and Miller, Todd and Jedrzejewski, Robert and Hack, Warren and Davis, David and Crawford, Steven and Law, D...

  75. [75]

    and Agol, Eric , doi =

    Cowan, Nicolas B. and Agol, Eric , doi =. Inverting. , keywords =

  76. [76]

    and Chayes, Victoria and Bouffard, \'Elie and Meynig, Max and Haggard, Hal M

    Cowan, Nicolas B. and Chayes, Victoria and Bouffard, \'Elie and Meynig, Max and Haggard, Hal M. , doi =. Odd. , keywords =

  77. [77]

    and Quanz, S

    Stolker, T. and Quanz, S. P. and Todorov, K. O. and Kühn, J. and Mollière, P. and Meyer, M. R. and Currie, T. and Daemgen, S. and Lavie, B. , doi =. , keywords =

  78. [78]

    The Journal of Open Source Software , keywords =

    Buchner, Johannes , doi =. The Journal of Open Source Software , keywords =

  79. [79]

    Phillips, M. W. and Tremblin, P. and Baraffe, I. and Chabrier, G. and Allard, N. F. and Spiegelman, F. and Goyal, J. M. and Drummond, B. and Hébrard, E. , doi =. A new set of atmosphere and evolution models for cool. , keywords =

  80. [80]

    J., Almaini, O., et al

    , keywords =. doi:10.1111/j.1365-2966.2007.12481.x , eprint =

    work page doi:10.1111/j.1365-2966.2007.12481.x 2007

Showing first 80 references.