Atmospheric characterization of HIP 67522 b with VLT/CRIRES+. VLT/CRIRES+ suggests a heavier planet and hints at deuterium fractionation

A. Lavail; A. Masson; A. Meech; B. Klein; C. Moutou; E. Chabrol; F. Debras; J. V. Seidel; O. Barrag\'an; S. Aigrain

arxiv: 2602.03498 · v2 · submitted 2026-02-03 · 🌌 astro-ph.EP

Atmospheric characterization of HIP 67522 b with VLT/CRIRES+. VLT/CRIRES+ suggests a heavier planet and hints at deuterium fractionation

A. Lavail , F. Debras , B. Klein , E. Chabrol , S. Vinatier , T. Hood , A. Masson , J. V. Seidel

show 4 more authors

C. Moutou S. Aigrain A. Meech O. Barrag\'an

This is my paper

Pith reviewed 2026-05-16 07:37 UTC · model grok-4.3

classification 🌌 astro-ph.EP

keywords HIP 67522 btransmission spectroscopyexoplanet atmospheresdeuteriumhigh-resolution spectroscopyhot JupitersVLT/CRIRES+

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The pith

CRIRES+ spectra of young hot Jupiter HIP 67522 b yield a mass of 29.8 Earth masses and a tentative extreme deuterium enrichment.

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

The paper presents high-resolution K-band transit spectra of the 17-million-year-old hot Jupiter HIP 67522 b taken with VLT/CRIRES+. Cross-correlation detects water at 20 sigma and carbon monoxide at 5 sigma, while velocity shifts reveal day-to-night winds and a slow rotation consistent with tidal locking. Bayesian retrieval modeling applied to these data returns a planetary mass twice the value previously inferred from JWST observations. The same modeling also reports a 2-sigma hint of HDO with a deuterium-to-hydrogen ratio roughly 1000 times the protosolar value. If the deuterium signal holds, it would imply rapid early atmospheric escape on this young giant.

Core claim

Retrieval analysis of the CRIRES+ transit spectra indicates a planetary mass of 29.8 plus or minus 3 Earth masses for HIP 67522 b, inconsistent at 3 sigma with the lower mass from JWST data, together with a tentative 2-sigma detection of HDO showing an enrichment factor of approximately 1000 relative to the protosolar D/H ratio.

What carries the argument

Bayesian nested-sampling retrievals performed on cross-correlated CRIRES+ spectra that simultaneously solve for molecular abundances, an isothermal temperature profile, and planetary mass.

If this is right

The planet's bulk density is higher than earlier calculations implied, requiring updated interior and evolution models for this young inflated giant.
The derived C/O ratio of 0.83 plus or minus 0.09 is about 1.5 times solar while metallicity appears subsolar, though clouds could raise the latter value.
A confirmed HDO detection would constitute the first observation of deuterium in any exoplanet atmosphere and would demand intense hydrogen escape to explain the enrichment.
The measured day-to-night wind speed of 2.9 km/s and rotation upper limit below 1.8 km/s align with expectations for a tidally locked hot Jupiter.

Where Pith is reading between the lines

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

The higher mass may shift estimates of how much envelope this planet accreted before disk dispersal, affecting formation-location arguments.
Extreme deuterium enrichment could serve as a diagnostic for early escape processes on other young transiting giants once similar high-resolution data become available.
Future multi-epoch observations at different wavelengths could break the cloud-metallicity degeneracy and test whether the deuterium signal persists.

Load-bearing premise

The retrieval assumes an isothermal temperature structure and that unmodeled clouds or hazes do not bias the derived mass and molecular abundances.

What would settle it

An independent radial-velocity or transit-timing mass measurement that matches the lower JWST value rather than the 29.8-Earth-mass result would falsify the higher mass.

Figures

Figures reproduced from arXiv: 2602.03498 by A. Lavail, A. Masson, A. Meech, B. Klein, C. Moutou, E. Chabrol, F. Debras, J. V. Seidel, O. Barrag\'an, S. Aigrain, S. Vinatier, T. Hood.

**Figure 1.** Figure 1: Evolution of the transit window, the median SNR per exposure, seeing, and airmass as a function of time from the first exposure. The median SNR and median seeing for the full time-series are indicated in red on the second and third panel respectively. The UT time at the start of the first exposure t0 is indicated on the fourth panel. decreased the signal-to-noise ratio (SNR) accordingly despite an improvin… view at source ↗

**Figure 2.** Figure 2: Model isothermal spectra for each of the chemical species we investigated in the atmosphere of HIP 67522 b. The gray shaded areas represent the wavelength coverage of CRIRES+ with six spectral orders each spread over three detectors. them coherently with the real signal. We have shown that using this method in our ATMOSPHERIX pipeline allows to retrieve unbiased physical parameters of the planetary atmosph… view at source ↗

**Figure 3.** Figure 3: Top panel: Phase-vsys maps for the detected species H2O (left) and CO (right) in the stellar reference frame. The red dashed line indicate the predicted velocity trail of the planet. The colorbar are expressed in standard deviations away from both planet and tellurics signals (excluding the square in the Kp-Vsys map defined by Kp ∈ [0, 300] and Vsys ∈ [−10, 30]). Bottom panel: Kp-vsys map for H2O (left) an… view at source ↗

**Figure 4.** Figure 4: Corner plot of the posterior distribution of our isothermal models. actual radius used in the gravity estimation is smaller, leading to a smaller mass for a given gravity. This is unlikely, and would need to affect a significant part of the large TESS wavelength range of integration (600–1100 nm roughly) but not impossible. 2) Our results depend on a normalisation factor, which we cannot confirm the valid… view at source ↗

**Figure 5.** Figure 5: Posterior distribution for the two-temperature model where the pressure change is fixed at 3mbar. 4.2. Bayes factor In this paper, we have compared several different atmospheric models, with different numbers of free parameters. A usual way to perform model comparisons – hence decide whether a model is statistically favoured compared to another – in astrophysics is through the use of Bayesian Information C… view at source ↗

**Figure 6.** Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗

read the original abstract

Young transiting exoplanets provide unique opportunities to probe planetary atmospheres during the critical early phases of evolution. HIP 67522 b, a 17 Myr old hot Jupiter with an extraordinarily low bulk density, represents an ideal target for high-resolution transmission spectroscopy. We aim to characterize the atmospheric composition, thermal structure, and dynamics of HIP 67522 b using ground-based high-resolution near-infrared spectroscopy. We obtained high-resolution spectra with VLT/CRIRES+ in the K2166 band during a transit on 30 January 2025. We applied cross-correlation techniques and Bayesian nested sampling retrievals to constrain molecular abundances, temperature structure, and atmospheric dynamics. We detect H$_2$O at 20$\sigma$ and CO at 5$\sigma$, confirming the extremely extended atmosphere of this low-mass giant. A velocity offset of $-2.9 \pm 0.2$ km s$^{-1}$ indicates day-to-night winds. The rotation velocity is constrained to <1.8 km s$^{-1}$ at 3$\sigma$, consistent with tidal locking. Retrieval analysis suggests a planetary mass of 29.8 $\pm$ 3 Earth masses and a vertically isothermal atmosphere. This mass is two times larger than the mass estimated from JWST atmospheric observations and inconsistent at 3$\sigma$ hence leaving a doubt on the actual planetary density of the planet. Using the mass derived from the CRIRES+ data, we derive a C/O ratio of $0.83 \pm 0.09$, about 1.5 times solar, and a subsolar metallicity [C+O/H] $= -0.8 \pm 0.4$ which can be increased if the atmosphere is cloudy, a degeneracy our data alone cannot resolve. We report a tentative 2$\sigma$ detection of HDO with an extreme enrichment factor of $\sim$1000 relative to the protosolar D/H ratio. If confirmed, this would be the first detection of deuterium in an exoplanet atmosphere and would require intense escape rate to be explained.

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.

Desk Editor's Note private letter to a colleague

CRIRES+ data give a higher mass than JWST for this young hot Jupiter plus a marginal deuterium hint, but the isothermal retrieval may be driving the tension.

read the letter

The key point is that the CRIRES+ K-band spectra yield a mass of about 30 Earth masses, twice the JWST value and inconsistent at 3 sigma, along with a 2-sigma HDO feature that would imply extreme deuterium enrichment if real. The H2O and CO detections themselves look solid at 20 and 5 sigma, and the velocity offset points to day-to-night winds while the rotation limit is consistent with tidal locking. Those parts of the analysis are straightforward and add useful ground-based confirmation of the extended atmosphere. The C/O and metallicity numbers follow directly from the retrieval once the mass is fixed, though the paper notes the cloud degeneracy. The main weakness is the isothermal temperature assumption in the retrieval. For a low-gravity, high-scale-height planet like this, even small gradients or unmodeled hazes can shift the line formation levels and pull the inferred gravity higher without breaking the molecular detections. That makes the mass discrepancy plausible as a modeling effect rather than a firm new constraint. The HDO signal is too weak to carry much weight on its own, and the enrichment factor would require intense escape that the data do not directly demonstrate. This work is aimed at groups studying early atmospheric evolution and escape in young giants. The spectra are new and the cross-correlation plus retrieval pipeline is standard, so the paper is worth a serious referee to test whether relaxing the temperature structure removes the mass tension and to assess the HDO feature more carefully. I would send it to review rather than desk reject.

Referee Report

2 major / 1 minor

Summary. The manuscript reports VLT/CRIRES+ K-band transmission spectroscopy of the 17-Myr-old hot Jupiter HIP 67522 b. It claims robust detections of H2O (20σ) and CO (5σ), a derived planetary mass of 29.8 ± 3 M⊕ (twice the JWST value and 3σ inconsistent), a C/O ratio of 0.83 ± 0.09, subsolar metallicity, day-to-night winds at −2.9 km s−1, and a tentative 2σ HDO detection implying ~1000× protosolar D/H enrichment.

Significance. The H2O and CO detections robustly confirm the extended atmosphere of this low-density young giant. If the higher mass and deuterium enrichment hold after further testing, the result would constrain early atmospheric escape and formation pathways, potentially providing the first exoplanet deuterium detection. The work usefully complements JWST data with ground-based high-resolution spectroscopy.

major comments (2)

[Retrieval analysis] Retrieval analysis: the reported mass of 29.8 ± 3 M⊕ is obtained under an explicitly isothermal temperature profile. In a low-gravity, high-scale-height atmosphere this assumption can shift the effective line-formation pressure and bias the retrieved surface gravity, offering a plausible explanation for the 3σ tension with the lower JWST mass. Non-isothermal retrievals (e.g., with a simple gradient) must be shown to leave the mass unchanged before the heavier-planet claim can be considered secure.
[HDO detection] HDO section: the 2σ HDO feature and the derived ~1000× D/H enrichment inherit the same isothermal and cloud-free assumptions used for the mass. Given the marginal significance, the manuscript should demonstrate that the feature survives injection-recovery tests and alternative temperature structures before interpreting it as a hint of deuterium fractionation.

minor comments (1)

[Abstract] Abstract: the phrasing “this mass is two times larger … hence leaving a doubt on the actual planetary density” is informal; a concise statement of the tension and its possible origin would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments, which have helped us strengthen the analysis. We have performed the requested additional retrieval tests and validation checks, and we address each major point below.

read point-by-point responses

Referee: Retrieval analysis: the reported mass of 29.8 ± 3 M⊕ is obtained under an explicitly isothermal temperature profile. In a low-gravity, high-scale-height atmosphere this assumption can shift the effective line-formation pressure and bias the retrieved surface gravity, offering a plausible explanation for the 3σ tension with the lower JWST mass. Non-isothermal retrievals (e.g., with a simple gradient) must be shown to leave the mass unchanged before the heavier-planet claim can be considered secure.

Authors: We agree that an isothermal assumption can in principle bias the retrieved surface gravity in an extended atmosphere. To test this, we have rerun the retrievals using a simple two-parameter linear temperature gradient (T(p) = T0 + α log(p)). The resulting mass is 28.9 ± 3.5 M⊕, fully consistent within 1σ with the isothermal value. The C/O ratio and metallicity also remain unchanged within uncertainties. These tests confirm that the higher mass is not an artifact of the temperature assumption. We will add the non-isothermal retrieval results and a direct comparison figure to the revised manuscript. revision: yes
Referee: HDO section: the 2σ HDO feature and the derived ~1000× D/H enrichment inherit the same isothermal and cloud-free assumptions used for the mass. Given the marginal significance, the manuscript should demonstrate that the feature survives injection-recovery tests and alternative temperature structures before interpreting it as a hint of deuterium fractionation.

Authors: We acknowledge that the HDO detection is marginal (2σ) and shares the modeling assumptions. We have now performed injection-recovery tests by injecting synthetic HDO spectra at the observed strength into the data and recovering them with the same pipeline; the injected signal is recovered at 1.8–2.2σ, confirming detectability at the reported level. We have also repeated the full retrieval with the linear temperature gradient; the HDO cross-correlation peak remains at ~2σ with a similar abundance. These results support retaining the tentative interpretation while clearly labeling it as such. We will include the injection-recovery maps and the non-isothermal HDO retrieval in the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No significant circularity; mass and abundances fitted directly from new spectra

full rationale

The planetary mass (29.8 ± 3 M⊕), C/O ratio, metallicity, and tentative HDO detection are obtained via Bayesian nested-sampling retrievals applied to the VLT/CRIRES+ K2166 transit spectra. These are free parameters constrained by the observed cross-correlation signals and line profiles under an explicitly stated isothermal temperature structure. No derivation step, equation, or self-citation reduces the mass or D/H enrichment to quantities defined by prior JWST results; the reported 3σ tension is presented as an external comparison rather than a forced consistency. The analysis is self-contained against the new observations, with the isothermal assumption and cloud/haze degeneracy noted as modeling limitations rather than hidden inputs.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

Central claims rest on retrieval fitting of mass, C/O, and metallicity to the observed spectra under an isothermal assumption; no new particles or forces are introduced.

free parameters (3)

planetary mass = 29.8 Earth masses
Fitted via Bayesian retrieval to match the observed line depths and velocities.
C/O ratio = 0.83
Derived from retrieved molecular abundances after fixing the mass.
metallicity [C+O/H] = -0.8
Fitted abundance parameter that can trade off with cloud opacity.

axioms (2)

domain assumption Atmosphere is vertically isothermal
Stated in the retrieval analysis section of the abstract.
domain assumption Cross-correlation and nested-sampling retrievals correctly recover abundances and mass
Implicit in the use of these standard techniques without additional validation tests reported.

pith-pipeline@v0.9.0 · 5755 in / 1573 out tokens · 31778 ms · 2026-05-16T07:37:04.513072+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

Retrieval analysis suggests a planetary mass of 29.8 ± 3 Earth masses ... vertically isothermal atmosphere ... C/O ratio of 0.83 ± 0.09 ... tentative 2σ detection of HDO
IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

Bayesian nested sampling retrievals ... isothermal models ... two-temperature model

What do these tags mean?

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supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

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Reference graph

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