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K-band spectra of five ultra-hot Jupiters are dominated by CO emission; thermal dissociation blocks reliable C/O ratios from this bandpass alone.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-07-11 22:28 UTC pith:DLVIBCPV

load-bearing objection Solid uniform KPIC K-band sample of six UHJs with three new detections; morphology claim holds, C/O limits correctly flagged. the 2 major comments →

arxiv 2607.03992 v1 pith:DLVIBCPV submitted 2026-07-04 astro-ph.EP

Atmospheric characterization of six ultra-hot Jupiters from K-band high-resolution spectroscopy

Luke Finnerty , Michael P. Fitzgerald , Yinzi Xin , Jerry W. Xuan , Julie Inglis , Shubh Agrawal , Ashley Baker , Randall Bartos
show 22 more authors
Geoffrey A. Blake Benjamin Calvin Sylvain Cetre Jacques-Robert Delorme Greg Doppmann Daniel Echeverri Katelyn Horstman Chih-Chun Hsu Nemanja Jovanovic Joshua Liberman Ronald A. L\'opez Dimitri Mawet Evan Morris Jacklyn Pezzato-Rovner Jean-Baptiste Ruffio Ben Sappey Tobias Schofield Andrew Skemer J. Kent Wallace Nicole L. Wallack Jason J. Wang Ji Wang
This is my paper
classification astro-ph.EP
keywords exoplanet atmospheresultra-hot Jupitershigh-resolution spectroscopyatmospheric retrievalthermal dissociationC/O ratioK-band emission
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper reports new Keck/KPIC high-resolution K-band detections of three ultra-hot Jupiters and a tentative detection of a fourth, then re-analyzes two earlier targets under a single retrieval pipeline. For five of the six planets the retrieved emission spectra are dominated by carbon monoxide, with only weak water or OH features that match the expected thermal breakup of H2O high in the atmosphere. The sixth, far hotter object shows almost no molecular signal. Free-chemistry and chemical-equilibrium retrievals both return carbon and oxygen abundances between one and ten times solar, yet the same dissociation that weakens the oxygen lines leaves the C/O ratio poorly constrained. The authors conclude that K-band data alone are insufficient for bulk composition and that broader wavelength and orbital-phase coverage will be required to pin down oxygen carriers and possible day–night inhomogeneities.

Core claim

Except for the hottest target KELT-9b, the six ultra-hot Jupiters observed with KPIC have K-band thermal-emission spectra dominated by CO emission features, accompanied by weak H2O or OH features consistent with thermal dissociation of water; the retrieved C and O abundances lie between 1 and 10 times solar, but dissociation prevents reliable C/O constraints from this bandpass alone.

What carries the argument

A uniform nested-sampling retrieval that fits a four-parameter Guillot pressure–temperature profile, orbital and rotational velocities, and free abundances of CO, H2O, OH and Fe, while imposing a Parmentier-style analytic vertical mixing profile for H2O (and a simple power-law profile for OH) so that thermal dissociation is accounted for without assuming full chemical equilibrium.

Load-bearing premise

That a simple one-dimensional temperature profile plus an analytic water-dissociation curve is enough to capture the real vertical and day–night structure once continuum information has already been removed by median division and PCA.

What would settle it

A joint retrieval of the same planets that adds H- or L-band data and recovers a tightly constrained C/O ratio inconsistent with the K-band-only posteriors, or shows that the CO and H2O emission peaks are systematically offset by more than a few km/s.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • UHJs with equilibrium temperatures between roughly 2200 K and 3000 K should share CO-dominated K-band emission spectra with only residual water or OH.
  • C/O and metallicity inferences drawn from K-band data alone for this population remain unreliable until dissociation is independently constrained.
  • Expanding wavelength coverage to the H or L band is required to break the abundance–temperature degeneracy and place useful limits on oxygen carriers.
  • Phase-resolved observations spanning both pre- and post-eclipse will be needed to separate Keplerian motion from possible day–night wind and abundance offsets.

Where Pith is reading between the lines

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

  • Once wider-band data exist, the same pipeline could be used to test whether the refractory-to-volatile ratio is systematically super-solar, a formation diagnostic left open by the present C/O scatter.
  • The weak or absent molecular signal from KELT-9b suggests a temperature threshold near 4000 K beyond which even CO is largely dissociated, offering a natural boundary for molecular versus atomic retrieval strategies.
  • Kinematic offsets already visible between single-molecule cross-correlation maps imply that future codes must allow species-dependent velocity fields if abundances are not to be biased.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. The paper reports new Keck/KPIC K-band high-resolution detections of three ultra-hot Jupiters (WASP-189b, MASCARA-1b, TOI-1518b) plus a tentative detection of KELT-9b, and reanalyzes prior KPIC data for WASP-33b and KELT-20b under a uniform free-chemistry and chemical-equilibrium retrieval framework. Free retrievals fit Guillot P–T parameters, kinematic offsets, rotational broadening, and abundances of CO, H2O, OH, and Fe with Parmentier-style parameterized vertical mixing for H2O/OH; equilibrium retrievals fit [C/H], [O/H], and [M/H]. Except for the much hotter KELT-9b, the retrieved spectra are CO-dominated beyond 2.3 µm with weak H2O/OH features consistent with thermal dissociation; carbon and oxygen abundances from detected species are 1–10× solar, but dissociation and continuum loss prevent reliable C/O constraints from K-band data alone. The authors conclude that wider wavelength and phase coverage are required.

Significance. Uniform multi-object KPIC analyses of UHJs remain rare; the paper supplies new detections, a consistent free-versus-equilibrium comparison, single-molecule Kp–Δvsys maps, and an explicit demonstration that nearly identical CO-dominated spectra can arise from widely different C/O posteriors. The free/equilibrium consistency checks, the mean-molecular-weight prior, and the transparent discussion of continuum and dissociation degeneracies are genuine strengths. If the morphology claim holds, the work usefully calibrates expectations for K-band-only UHJ retrievals and motivates joint optical/IR or H+K analyses.

major comments (2)
  1. §3.3 and Fig. 9: The free-chemistry KELT-9b solution prefers an H2O-dominated spectrum that the authors themselves flag as inconsistent with chemical expectations and with literature (optical Fe, SPIRou Fe/OH/CO). The equilibrium retrieval recovers a more plausible Fe/CO atmosphere at SNR = 5.0. Because the abstract and summary statements treat KELT-9b as a distinct (molecule-poor) case, the free-retrieval H2O solution should either be demoted more clearly to a cautionary example of low-SNR failure or the bluest-order omission tests should be elevated to the fiducial result for this target.
  2. §2.3.4–2.3.5 and Figs. 5–8: Continuum information is lost to median division/PCA; the log-normal scale-factor prior only partially breaks the temperature–abundance degeneracy. The paper already shows continuum levels differing from blackbody expectations by factors of ~2–4 and free/equilibrium C/O posteriors that can flip while producing nearly identical spectra. The central claim that C/O cannot be recovered from K-band alone is therefore well supported, but the reported 1–10× solar abundance range remains prior- and parameterization-dependent; a short quantitative sensitivity test (e.g., relaxing the MMW penalty or the scale-factor prior width) would strengthen the abundance statements.
minor comments (6)
  1. Abstract and §1: SNR values quoted for the new detections (7.2, 8.6, 7.1, 5.0) do not always match the Kp–Δvsys SNRs in Fig. 3 (e.g., KELT-9b listed as 5.0 vs. 6.7). Clarify which metric is used throughout.
  2. Table 1 note and §2.1.6: The adopted Kp = 198 km s−1 for TOI-1518b is an ad-hoc average of discrepant literature values; state the impact on the retrieved ΔKp posterior more explicitly.
  3. §2.3.1: The choice of six PCA components is justified by residual inspection, but a brief quantitative comparison (e.g., Δlog Z or residual variance) across 4/6/8 components for the weaker detections would help readers assess robustness.
  4. Fig. 6: The blackbody comparison curves are useful; adding the contribution-function-weighted continuum or a simple H−-included model for the hottest targets would make the continuum discrepancy discussion more concrete.
  5. Typographical: “Except for \knb” in the abstract appears to be a macro error; several sentences in §3.1–3.2 repeat “the the”.
  6. §4.3: The discussion of kinematic offsets correctly notes that ephemeris and LSF uncertainties preclude wind measurements; a short statement of the expected systematic floor (~4–5 km s−1 from LSF) would help non-specialists.

Circularity Check

0 steps flagged

No significant circularity: observational detections and free/equilibrium retrievals rest on new KPIC spectra plus external parameterizations (Guillot, Parmentier); self-citations are methodological background only.

full rationale

The paper's load-bearing claims (CO-dominated K-band emission for five UHJs, weak H2O/OH consistent with dissociation, 1–10× solar C/O-bearing abundances, and inability to constrain C/O from K-band alone) are obtained by applying a standard nested-sampling retrieval (petitRADTRANS + MultiNest + Gibson log-likelihood) to newly reduced KPIC time series. The Guillot P–T form, Parmentier analytic H2O mixing profile, and power-law OH profile are taken from external literature and used as flexible parameterizations whose free parameters are fitted to the data; free-versus-equilibrium consistency checks (Figs. 6–8) and single-molecule Kp–Δvsys maps (Fig. 4) then demonstrate the resulting degeneracies rather than assuming them away. Self-citations (Finnerty et al. 2023, 2025a,b) supply only the reduction pipeline, LSF scaling, and prior choices; they do not define the reported SNRs, abundances, or spectral morphology. No fitted quantity is re-labeled a prediction, no uniqueness theorem is imported, and no ansatz is smuggled as a derivation. The analysis is therefore self-contained against the new spectra and external tools; the minor self-citation score of 1 reflects ordinary methodological continuity, not circular reduction of the central claims.

Axiom & Free-Parameter Ledger

4 free parameters · 5 axioms · 0 invented entities

The paper is an observational retrieval study. Load-bearing free parameters are the usual atmospheric-retrieval set (Guillot P–T coefficients, molecular VMRs or elemental abundances, kinematic offsets, scale factor). Domain assumptions include 1-D radiative transfer, the analytic Parmentier H2O dissociation profile, neglect of H− opacity, and the effectiveness of PCA + median division. No new physical entities are invented.

free parameters (4)
  • Guillot P–T parameters (log κ, log γ, Tint, Tequ)
    Four free parameters that set the temperature structure; poorly constrained in absolute temperature but control thermal contrast and therefore line strengths.
  • log VMRs of H2O, 12CO, OH, Fe, 13CO (free retrieval) or [C/H], [O/H], [M/H] (equilibrium)
    Primary abundance parameters whose posteriors are the central compositional results; subject to dissociation–abundance degeneracies.
  • ΔKp, Δvsys, vrot, scale factor
    Kinematic and continuum-scale parameters fitted simultaneously; scale factor prior is log-normal with σ=0.1 to partially break temperature–abundance degeneracy.
  • Number of PCA components omitted (fiducial = 6)
    Chosen by visual inspection of residuals; posteriors are shown to be stable for 4/6/8 components but still a discrete analysis choice.
axioms (5)
  • domain assumption 1-D plane-parallel atmosphere with Guillot (2010) analytic P–T profile is an adequate description for dayside emission retrievals
    Section 2.3.4; free-node P–T tests were unconstrained, so Guillot form is adopted.
  • domain assumption Parmentier et al. (2018) analytic expression plus power-law OH profile captures vertical mixing of H2O and OH under dissociation
    Section 2.3.5; free dissociation-pressure retrievals were unconstrained for most targets.
  • domain assumption H− continuum opacity can be omitted in the K band without biasing relative line strengths
    Section 2.3.8; justified by free-free nature producing only a uniform scaling that HRCCS is insensitive to.
  • domain assumption PCA + median division + Gibson (2020) likelihood correctly removes stellar/telluric signals while preserving planetary information
    Section 2.3.1–2.3.2; standard HRCCS practice, validated by multi-PC consistency checks.
  • ad hoc to paper Mean-molecular-weight penalty (Gaussian above 2.8 amu) prevents unphysical metal-rich solutions
    Section 2.3.5; introduced to keep atmospheres H2-dominated while still allowing high metallicity.

pith-pipeline@v1.1.0-grok45 · 56774 in / 3008 out tokens · 28705 ms · 2026-07-11T22:28:20.906827+00:00 · methodology

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read the original abstract

We present new Keck/KPIC high-resolution spectroscopic detections of three ultra-hot Jupiters (UHJs) in the $K$ band: WASP-189b ($\rm SNR = 7.2$), MASCARA-1b ($\rm SNR = 8.6$), and TOI-1518b ($\rm SNR = 7.1$), as well as a tentative detection of KELT-9b ($\rm SNR = 5.0$). We perform a uniform set of atmospheric retrieval analysis on these objects, as well as previously reported KPIC observations of WASP-33b ($\rm SNR = 11.2$) and KELT-20b ($\rm SNR = 10.5$), We perform atmospheric retrievals for the pressure-temperature ($P-T$) profile, orbital velocity parameters, $v\sin i$, and abundances of CO, H$_2$O, OH, and Fe, with parameterized mixing profiles to account for the expected vertical abundance variations of H$_2$O and OH. We also perform a set of retrievals assuming chemical equilibrium, which are generally in good agreement with the free retrievals. Except for \knb, the retrieved spectra are dominated by CO emission features, with additional weak H$_2$O or OH features consistent with thermal dissociation of H$_2$O. \knb, which is significantly hotter, appears to have very weak molecular features. Dissociation limits our ability to reliably constrain H$_2$O or OH abundances from $K$ band data alone, resulting in poor constraints on the C/O ratio. For all objects, the atmospheric abundances from detected carbon and oxygen species are $1-10\times$ solar. These results highlight the importance of wide spectral coverage for high-resolution retrievals. Additional observations to expand phase and wavelength coverage are needed to better constrain oxygen species and possible spatial inhomogeneities from dissociation.

Figures

Figures reproduced from arXiv: 2607.03992 by Andrew Skemer, Ashley Baker, Benjamin Calvin, Ben Sappey, Chih-Chun Hsu, Daniel Echeverri, Dimitri Mawet, Evan Morris, Geoffrey A. Blake, Greg Doppmann, Jacklyn Pezzato-Rovner, Jacques-Robert Delorme, Jason J. Wang, Jean-Baptiste Ruffio, Jerry W. Xuan, Ji Wang, J. Kent Wallace, Joshua Liberman, Julie Inglis, Katelyn Horstman, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Nicole L. Wallack, Randall Bartos, Ronald A. L\'opez, Shubh Agrawal, Sylvain Cetre, Tobias Schofield, Yinzi Xin.

Figure 1
Figure 1. Figure 1: Orbital phase coverage of our observations, with semi-major axes drawn to-scale. The stellar radii are shown as dashed vertical lines in the colors corresponding to each planet to illustrate the start/end of secondary eclipse. We omit portions of the time series for TOI-1518 b, WASP-33 b, WASP-189 b, and KELT-9 b falling within secondary eclipse. WASP-33 b, KELT-9 b, and MASCARA-1 b were observed to signif… view at source ↗
Figure 2
Figure 2. Figure 2: Time series log-likelihoods in the nominal planet rest frame computed for each frame (top) and summed in the planet reference frame (bottom) for each target and time series. The nominal planet reference frame is indicated in dotted red, the stellar reference frame in solid black, and the telluric reference frame in dashed black. In the lower panel, individual orders are shown in blue, while the sum of all … view at source ↗
Figure 3
Figure 3. Figure 3: Kp − ∆vsys diagrams for the free retrieval maximum-likelihood model for each target, omitting six principal com￾ponents. The maps are computed with the log-likelihood function, and converted to signal-to-noise by first median-subtracting each row of constant Kp and then dividing by the standard deviation of the Kp< 0 region. The nominal planetary Kp and ∆vsys are indicated in dashed red, and the red dot in… view at source ↗
Figure 4
Figure 4. Figure 4: Kp − ∆vsys contours for the free retrieval maximum-likelihood model (black) as well as CO-only (filled dark red), H2O-only (filled blue) and OH-only (filled cyan) models. Each model was generated using the retrieved maximum-likelihood parameters, setting the abundance of the included species to 10−3 and the abundances of all other species to 10−15. The contours are drawn at SNR = 2, 4, 6. The contours enab… view at source ↗
Figure 5
Figure 5. Figure 5: Retrieved P − T profiles for each target. The median profiles are shown in green and maximum-likelihood are shown in purple, with the free retrievals shown as solid lines and the equilibrium as dashed lines. The black lines show 500 draws from the posterior. The black line to the right shows the wavelength-median emission contribution function for the maximum-likelihood profile from the free retrieval. Str… view at source ↗
Figure 6
Figure 6. Figure 6: Planet/star flux ratios for the free retrieval maximum-likelihood (purple) free retrieval median (green), equilibrium max-likelihood (cyan), and equilibrium median (yellow) planet models, compared with a blackbody (dashed blue). Observed NIRSPEC orders are shaded. All retrieved spectra except KELT-9 b are dominated by emission from the 12CO ν = 2 − 0 band beyond 2.3 µm, with features from mostly H2O or OH … view at source ↗
Figure 7
Figure 7. Figure 7: Retrieved max-likelihood P −T profiles (black) and volume mixing ratios for H2O (blue), CO (dark red), OH (cyan), and Fe (light orange) for all targets. The free retrievals are shown as solid lines while the equilibrium retrievals are shown as dashed lines. The gray lines at the right show the wavelength-median emission contribution function. KELT-9 b shows the largest discrepancy between the retrievals, w… view at source ↗
Figure 8
Figure 8. Figure 8: Derived posteriors for the C/O ratio, carbon and oxygen abundances, total volatile abundance, and iron abundance. Median and ±34% confidence intervals are indicated in solid and dotted red, respectively, and the solar values are shown in dash-dot black. The black distribution is computed from the free retrieval, and the blue distribution from the equilibrium retrieval. The retrieved carbon and oxygen abund… view at source ↗
Figure 9
Figure 9. Figure 9: Left: Kp − ∆vsys map for KELT-9 b, similar to [PITH_FULL_IMAGE:figures/full_fig_p022_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: C/O versus volatile abundance (left), C/O versus planet mass and equilibrium temperature (upper row), and volatile abundance versus planet mass and equilibrium temperature (lower row). The free retrieval values are shown in black and the equilibrium retrievals in blue. The equilibrium values have been slightly offset in mass and temperature for clarity. None of these parameters appear to be significantly … view at source ↗
Figure 11
Figure 11. Figure 11: Full corner plot for KELT-20 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p032_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Full corner plot for WASP-33 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p033_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Full corner plot for KELT-9 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p034_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Full corner plot for WASP-189 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p035_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Full corner plot for MASCARA-1 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p036_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Full corner plot for TOI-1518 b. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3 [PITH_FULL_IMAGE:figures/full_fig_p037_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Full corner plot for the equilibrium retrievals. Red solid lines indicate the medians, while red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 3. Plots correspond, from left to right, top to bottom, KELT-20 b, WASP-33 b, KELT-9 b, WASP-189 b, MASCARA-1 b and TOI-1518 b, respectively [PITH_FULL_IMAGE:figures/full_fig_p038_17.png] view at source ↗

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