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REVIEW 3 major objections 5 minor 59 references

Retrieving wind properties from the ultra-hot dayside of WASP-189b with CRIRES$^+$

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The dayside wind of ultra-hot Jupiter WASP-189b is best explained by a day-to-night flow of about 4.4 km/s, with no detectable equatorial jet.

desk verdict A careful, honest retrieval paper whose headline wind detection is statistically marginal; worth a serious referee, but the abstract oversells and a model comparison is missing. read the letter →

arxiv 2411.19662 v1 pith:TUV4JI2F submitted 2024-11-29 astro-ph.EP

F. Lesjak , L. Nortmann , D. Cont , F. Yan , A. Reiners , N. Piskunov , A. Hatzes , L. Boldt-Christmas
show 7 more authors
S. Czesla A. Lavail E. Nagel A. D. Rains M. Rengel U. Seemann D. Shulyak
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetatmospheresultra-hotJupiterWASP-189bhigh-resolutionspectroscopyatmosphericcirculationday-to-nightwindequatorialjetemission
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 tries to establish how winds circulate in the upper atmosphere of WASP-189b, an ultra-hot gas giant with a dayside hot enough to melt iron. Using high-resolution K-band emission spectroscopy, the authors detect carbon monoxide and iron lines from the planet's dayside and fit their shapes with a model that separates three motions: the planet's tidally locked rotation, a uniform day-to-night flow, and a zonal equatorial jet. The best-fitting day-to-night wind is $4.4^{+1.8}_{-2.2}$ km/s, while the equatorial jet is only $1.0^{+0.9}_{-1.8}$ km/s and is consistent with zero. If correct, the roughly 6 km/s red-shift measured in the planet's lines is mostly gas streaming from the heated dayside toward the nightside, and the circulation is dominated by day-to-night flow rather than the fast equatorial jet predicted by some global circulation models.

What carries the argument

The argument is carried by a disk-integrated velocity-profile model. The projected dayside is divided into a fine grid of cells, each assigned a radial velocity from the tidally locked rotation, a constant day-to-night wind, and a Gaussian-shaped equatorial jet whose width is a free parameter; each cell is also brightness-weighted by a linear limb-darkening law. Histogramming the cell velocities weighted by brightness produces a line profile, which is convolved onto synthetic emission spectra in logarithmic wavelength space and fitted to the data after stellar and telluric lines are removed with a principal-component filter. A model-filter step reproduces the distortions that line removal introduces, and an injection test shows that the wind-induced broadening and the red-shifted wing survive that filtering. This replaces the simpler rigid-rotation profile with a wind screen, turning a velocity-offset measurement into a wind measurement.

What would settle it

Take high-resolution K-band dayside spectra over a wider orbital-phase range around secondary eclipse and measure the CO and Fe line-centre shift as a function of sub-stellar longitude. If the shift tracks the rotating hot region, the day-to-night wind interpretation is supported; if it stays constant near 2 km/s, the remaining offset is dominated by orbital-clock or systematic effects and the wind speed would be overestimated. A hot-spot-only retrieval, with the same grid but no wind, would settle whether the extended red wing truly requires a wind; the paper states such a comparison but does not show it.

Watch

Extended reading notes

Core claim

The central discovery is that the line shape of WASP-189b's dayside emission favours a wind pattern. The paper reports that the observed CO and Fe lines are best fitted when gas moves from the sub-stellar point toward the nightside at $4.4^{+1.8}_{-2.2}$ km/s across the visible hemisphere, while the retrieved equatorial jet velocity of $1.0^{+0.9}_{-1.8}$ km/s is consistent with the absence of a jet. Adding this wind reduces the unexplained velocity offset from about 4.7 km/s to $1.9^{+1.6}_{-1.5}$ km/s, so the wind explains most but not all of the red-shift; a stronger wind would produce more line broadening than observed. The same retrieval finds an inverted temperature-pressure profile and, under equilibrium chemistry, a C/O ratio of $0.32^{+0.41}_{-0.14}$ and a metallicity of $[M/H] = 1.40^{+1.39}_{-0.60}$, and the paper argues that a bright sub-stellar hot spot alone cannot reproduce the measured red-shifted wing.

Load-bearing premise

The load-bearing premise is that the visible dayside can be described by a single uniform day-to-night wind plus a Gaussian jet superimposed on a tidally locked, linearly limb-darkened disk with no sub-stellar hot spot; if the real velocity field contains a hot spot or spatially varying winds, the retrieved speeds and the residual velocity offset will be biased.

Editorial extensions

If this is right

  • A red-shift of a few km/s in a hot Jupiter's dayside spectrum can be produced by a day-to-night wind, so future detections of such offsets do not by themselves require unseen orbital or systematic errors.
  • Most of the roughly 6 km/s offset in WASP-189b's CO and Fe lines is wind, with a remaining offset of about 2 km/s that could come from orbital-clock uncertainties or a sub-stellar hot spot.
  • A near-zero equatorial jet supports the idea that extreme irradiation suppresses zonal jets in ultra-hot Jupiters, leaving day-to-night flow as the dominant circulation.
  • An inverted temperature-pressure profile and a stellar-to-super-solar metallicity, if confirmed, indicate a strongly irradiated, heavy-element-enriched atmosphere with thermal dissociation shaping the upper layers.
  • Combining transmission and dayside observations in one retrieval would use opposite wind shifts on the two hemispheres to constrain the velocity offset and wind speed more tightly than either data set alone.

Reading between the lines

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

  • A testable extension would be phase-resolved spectroscopy: if day-to-night flow dominates, the line-centre shift should track the sub-stellar longitude as the planet rotates, whereas a fixed ephemeris offset would not vary with phase.
  • The wind speed is mainly carried by the CO line shape because CO has the strongest signal; a retrieval on a wavelength setting with dominant Fe lines would test whether the wind geometry is uniform across species.
  • Because the model omits a bright sub-stellar spot and the paper does not show the hot-spot-only simulation, a natural next test is to add a spot brightness map; such a spot would also produce a red-shift, so part of the retrieved 4.4 km/s wind could trade against a spot-induced shift.
  • Since the posterior is consistent with no wind at about the 2-sigma level, the wind claim leans on the line-broadening side of the fit; a higher-signal-to-noise spectrum would decide between a 4 km/s wind plus small offset and a no-wind atmosphere with a large offset.
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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. The paper presents CRIRES+ K-band dayside emission spectroscopy of the ultra-hot Jupiter WASP-189b. After removing stellar and telluric lines with SYSREM, the authors detect CO and Fe with a velocity offset of about 6 km/s relative to the expected planetary rest frame. They then perform a Bayesian atmospheric retrieval with petitRADTRANS, and extend it with a disk-integrated line-profile model that includes tidally locked rotation, a uniform day-to-night wind, and a Gaussian-profile equatorial jet. They report a day-to-night wind speed of 4.4+1.8-2.2 km/s and an equatorial jet velocity consistent with zero, together with a reduced residual velocity offset, an inverted temperature-pressure profile, and equilibrium-chemistry C/O and metallicity constraints. The central interpretive claim is that the dayside circulation of WASP-189b is dominated by day-to-night flow rather than by a fast zonal jet as predicted by Lee et al. (2022).

Significance. If the wind detection is statistically robust, the result is an important empirical constraint on circulation in ultra-hot Jupiters, favoring day-to-night flows over zonal jets in WASP-189b and providing a direct test of general circulation models. The paper has several genuine strengths: the SYSREM filtering effect on line shapes is validated with injection tests in Appendix B, the number of SYSREM iterations is selected objectively following Cheverall et al. (2023), the reduced data are publicly available, and the authors openly discuss degeneracies and modelling limitations. The main significance is currently limited by the marginal statistical significance of the wind signal and by the simplified kinematic model used to interpret the line profile.

major comments (3)
  1. [Section 5.2 and Table C.1] The headline result that the line profile is 'best fitted' by a day-to-night wind is not supported by any quantitative model comparison. The retrieved vday-night = 4.4+1.8-2.2 km/s is consistent with zero at about the 2-sigma level, as the paper itself states, and voffset is a free parameter that can absorb part of the velocity shift. The authors should compare the wind retrieval against a no-wind model (vday-night fixed to zero, with voffset left free) using Bayesian evidence, BIC, or a likelihood-ratio test, and report the resulting significance. Until this is done, the abstract and Section 6 overstate the result.
  2. [Sections 5.1-5.2] The line-profile model assumes a uniform day-to-night wind over the entire visible hemisphere, no sub-stellar hot spot, and a linear limb-darkening law with a free coefficient epsilon. The retrieved epsilon is unconstrained, so the brightness weighting of the disk is largely free. The statement that 'a hot spot alone can not result in the retrieved line profile' is load-bearing for the wind interpretation, but the supporting simulations are not shown or referenced. Please include these simulations or an equivalent injection test with a hot-spot model, and quantify how much the retrieved vday-night and voffset shift when a hot spot or a spatially varying wind field is included.
  3. [Appendix C and Fig. C.1] The posteriors of sigma_jet and epsilon fill the entire prior range, and vjet is consistent with zero within uncertainties. This means the only constrained wind parameter is vday-night, while the two unconstrained parameters add flexibility to the line-profile model. The paper should state this limitation more prominently and, ideally, repeat the wind retrieval with sigma_jet and epsilon fixed to fiducial values to demonstrate that the vday-night constraint is stable under plausible choices of these nuisance parameters.
minor comments (5)
  1. [Abstract] The abstract should quote the 1-sigma uncertainties on the retrieved wind speeds, since their precision is central to the claim.
  2. [Tables 3 and C.1] The prior range for log10 kappa_IR differs between the initial retrieval ([-15, 4]) and the wind-pattern retrieval ([-5, 5]); please clarify whether this difference is intentional and whether it affects the comparability of the retrieved T-p parameters.
  3. [Appendix A] The appendix title refers to 'Kp-vsys maps', but the plotted quantity is voffset as defined in Eq. (2); retitle the appendix to 'Kp-voffset maps' for consistency.
  4. [Section 5.2] The sentence 'We were not able to place constrains on the limb darkening coefficient' contains a typo: 'constrains' should be 'constraints'.
  5. [Section 3.4] The claim that the CO and Fe signals are 'stable across a wider range of iterations' is not documented; a supplementary figure or a brief quantitative statement of the iteration range would make this assertion checkable.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the wind speeds are free parameters fitted to the data, and the paper's self-citations are methodological, not load-bearing.

full rationale

The derivation chain is self-contained. The wind parameters vday-night and vjet are free parameters in a forward model (Table C.1: vday-night prior [0,20] km/s, vjet prior [-20,20] km/s), fitted by MCMC against the CRIRES+ residual spectra; they are not constructed from the measured velocity offset or from any other retrieved quantity. The abstract's wording 'best fitted by the presence of a day-to-night wind' is a report of the posterior mode, not a prediction of an independent quantity. The line-profile model's day-to-night wind and jet prescriptions are explicitly introduced as assumptions in Sect. 5.1, not imported as established results. Self-citations (Lesjak et al. 2023 for PSF width, Cont et al. 2022 for CCF calculation, Boldt-Christmas et al. 2024 for SYSREM considerations) are methodological tools and are not load-bearing for the central wind claim. The paper also openly acknowledges the degeneracy between wind speed and velocity offset and states that the day-to-night wind posterior is consistent with a wind-free scenario to within ~2 sigma (Sect. 5.2); this is an honest statistical caveat, not circular reasoning. Any concern about statistical marginality or absence of formal model comparison is a correctness/evidence-quality issue, not a circularity issue.

Assumptions & free parameters 12 free parameters · 6 assumptions · 0 invented entities

The central claim rests on a forward model with 12 fitted parameters, a simplified wind geometry, equilibrium chemistry, and a filtering approximation. No new physical entities are introduced. The wind speeds themselves are fitted, not independently predicted, and the unconstrained jet width and limb darkening indicate the line profile model is underdetermined in parts.

free parameters (12)
  • Tirr = 3270 (+600, -530) K
    Retrieved irradiation temperature in the Guillot T-p profile; strongly degenerate with kappa_IR and gamma.
  • log10 kappa_IR = -0.9 (+0.5, -1.3)
    Retrieved infrared opacity; correlates with Tirr and gamma.
  • log10 gamma = 0.9 (+0.7, -0.2)
    Retrieved ratio of visible to infrared opacity; part of T-p structure.
  • Kp = 193.7 (+2.6, -2.5) km/s
    Retrieved orbital semi-amplitude; consistent with the literature value of 201 +/- 4 km/s.
  • voffset = 1.9 (+1.6, -1.5) km/s
    Residual velocity offset; degenerate with the day-to-night wind speed.
  • v_day-night = 4.43 (+1.80, -2.19) km/s
    Retrieved uniform day-to-night wind speed; the central fitted parameter of the wind study.
  • vjet = 1.02 (+0.93, -1.81) km/s
    Retrieved equatorial jet speed; consistent with no jet.
  • sigma_jet = 0.46 (+0.37, -0.36) Rp
    Retrieved jet width; unconstrained and fills the prior.
  • epsilon = 0.47 (+0.36, -0.33)
    Retrieved limb-darkening coefficient; unconstrained.
  • C/O = 0.26 (+0.32, -0.13)
    Retrieved carbon-to-oxygen ratio under equilibrium chemistry; consistent with solar.
  • [M/H] = 1.90 (+1.83, -0.95)
    Retrieved metallicity; consistent with solar within 2-3 sigma.
  • beta = 0.95 (nominal)
    Noise scaling factor in the likelihood; near unity, indicating well-calibrated uncertainties.
assumptions (6)
  • domain assumption Equilibrium chemistry (fastChem) sets all abundances from C/O and [M/H], with [Fe/H]=[O/H]=[N/H]=[M/H]
    Invoked in Sect. 4.1. If photoionization or other disequilibrium effects matter on the UHJ dayside, the retrieved chemistry and line strengths could be biased; the paper explicitly excludes disequilibrium.
  • domain assumption The T-p profile follows the Guillot (2010) parametric model with Tint fixed to 200 K
    Used in Sects. 3.1 and 4.1. The emission spectra are insensitive to deep layers; the chosen parametrization shapes the thermal inversion and thus the line emission.
  • domain assumption Planet is tidally locked with orbital-period rotation (max 3.0 km/s) and a linear limb-darkening brightness law
    Assumed in Sect. 5.1 when building the velocity profile. If rotation is not fully locked or the brightness map differs, the retrieved wind speeds would be biased.
  • ad hoc to paper Wind field is a uniform day-to-night wind plus a Gaussian-profile equatorial jet
    Defined in Sect. 5.1. Real circulation is spatially variable; the retrieved speeds are effective averages, as the authors acknowledge.
  • domain assumption The Gibson et al. (2022) model filter preserves line-shape differences between wind scenarios
    Validated in App. B for a single CO line and three scenarios; the retrieval applies it to all lines and a continuous parameter space.
  • domain assumption Observations at phases 0.53-0.57 are treated as full-dayside visibility with no nightside contribution
    Section 5.2; the nightside gradually rotates into view, which the model ignores. The authors state this is a small effect.

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Cite this review

Pith. "Pith review of Retrieving wind properties from the ultra-hot dayside of WASP-189b with CRIRES$^+$." pith.science (2026). https://pith.science/paper/TUV4JI2F

@misc{pith2026241119662,
  author       = {Pith},
  title        = {Pith review of: Retrieving wind properties from the ultra-hot dayside of WASP-189b with CRIRES$^+$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TUV4JI2F}},
  note         = {Machine review of arXiv:2411.19662}
}
abstract

The extreme temperature gradients from day- to nightside in the atmospheres of hot Jupiters generate fast winds in the form of equatorial jets or day-to-night flows. Observations of blue-shifted and red-shifted signals in the transmission and dayside spectra of WASP-189b have sparked discussions about the nature of winds on this planet. To investigate the structure of winds in the atmosphere of the ultra-hot Jupiter WASP-189b, we studied its dayside emission spectrum with CRIRES$^+$ in the spectral K band. We used the cross-correlation method to detect emission signals of CO and Fe, and employed a Bayesian framework to retrieve the atmospheric parameters relating to the temperature-pressure structure and chemistry. The retrieval incorporated a numerical model of the line profile influenced by various dynamic effects to determine the wind structure. The cross-correlation signals of CO and Fe showed a velocity offset of ~6km/s, which could be caused by a fast day-to-night wind in the atmosphere of WASP-189b. The atmospheric retrieval showed that the line profile of the observed spectra is best fitted by the presence of a day-to-night wind of 4.4km/s, while the retrieved equatorial jet velocity of 1.0km/s is consistent with the absence of such a jet. Such a wind pattern is consistent with the observed line broadening and can explain the majority of the velocity offset, while uncertainties in the ephemerides and the effects of a hot spot could also contribute to this offset. We further retrieved an inverted temperature-pressure profile and determined the C/O ratio and metallicity. We showed that red-shifts of a few km/s in the dayside spectra could be explained by day-to-night winds. Further studies combining transmission and dayside observations could advance our understanding of WASP-189b's atmospheric circulation by improving the uncertainties in the velocity offset and wind parameters.

Figures

Figures reproduced from arXiv: 2411.19662 by the authors.

Figure 1
Figure 1. Data reduction steps of a representative wavelength range. Top panel: Unprocessed spectra as they are produced by the CRIRES+ pipeline. Middle panel: After normalisation to bring all spectra onto a common blaze function, and masking of deep telluric lines. Bottom panel: After the removal of stellar and telluric lines with SYSREM. 3. Cross-correlation 3.1. Generating planetary model spectra We calculated synthetic mo… view at source ↗
Figure 2
Figure 2. S/N detection strength as a function of SYSREM iterations for the signal of CO, at nodding positions A (blue colour) and B (orange colour). The top panel shows the signal strength for the real data, and the bottom panel shows the strength of an injected signal using the dif￾ferential ∆CCF according to the method described in Sect. 3.3. The dia￾mond shapes indicate the SYSREM iteration with the strongest detection of… view at source ↗
Figure 3
Figure 3. Model spectra (top), cross-correlation functions (CCFs, middle)), and Kp-voffset maps (bottom) of CO, Fe and H2O. The dashed lines in the middle panels indicate the expected course of the planetary trail (which is located between the two lines). The signals of CO and Fe are visible in the CCFs and Kp-voffset maps, while H2O was not detectable. abundances for the retrieval and instead determined pressure￾dependent ab… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Posterior distributions from the retrieval of the atmospheric and orbital parameters. The dashed lines indicate the mean value and the 16th and 84th percentile. The included parameters consists of the three parameters defining the T-p profile (Tirr, κIR, γ), the orbita…
Figure 5
Figure 5. Figure 5: Retrieved temperature and abundance profiles. Left panel: Retrieved T-p profile calculated from 10 000 random samples. The shaded region indicates the 1σ uncertainty interval. Middle and right panel: Retrieved abundance profiles of the individual species as determined …
Figure 6
Figure 6. Figure 6: Examples of different radial velocity distributions on the planetary disk and resulting velocity profiles, and the result from the retrieval. The example profiles assume a limb darkening coefficient of ϵ = 1. a) Tidally locked rotation (according to WASP-189 b’s orbita…
Figure 7
Figure 7. Figure 7: Posterior distributions from the retrieval of the atmospheric and orbital parameters. The dashed lines indicate the mean value and the 16th and 84th percentile. The posteriors of the jet width σjet and limb darkening coefficient ϵ fill the entire parameter space and th…

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Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.