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PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio

T0 review · 2 major / 3 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read First abundance measurement of a planet still forming in its disk finds a stellar-like carbon-to-oxygen ratio.

desk verdict First molecular detections and C/O measurement for PDS 70b, but the C/O limit rests on a cloudless P-T profile the paper's own forward model disfavors. read the letter →

arxiv 2411.15117 v2 pith:4QSYTRQW submitted 2024-11-22 astro-ph.EP astro-ph.SR

Chih-Chun Hsu , Jason J. Wang , Geoffrey A. Blake , Jerry W. Xuan , Yapeng Zhang , Jean-Baptiste Ruffio , Katelyn Horstman , Julianne Cronin
show 22 more authors
Ben Sappey Yinzi Xin Luke Finnerty Daniel Echeverri Dimitri Mawet Nemanja Jovanovic Clarissa R. Do Ó Ashley Baker Randall Bartos Benjamin Calvin Sylvain Cetre Jacques-Robert Delorme Gregory W. Doppmann Michael P. Fitzgerald Joshua Liberman Ronald A. López Evan Morris Jacklyn Pezzato-Rovner Tobias Schofield Andrew Skemer J. Kent Wallace Ji Wang
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords protoplanetPDS70bcarbon-to-oxygenratiohigh-resolutionspectroscopyatmosphericretrievalplanetformationKPIC
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the first measurement of the atmospheric carbon-to-oxygen ratio of a protoplanet still embedded in its natal disk, using Keck/KPIC high-resolution spectroscopy. The authors detect carbon monoxide and water in PDS 70b and retrieve a C/O ratio of 0.28+0.20-0.12, consistent with the host star and lower than the carbon-rich outer disk gas. Because PDS 70b is the only confirmed planet still forming inside its birth disk, this measurement offers a direct test of how planets acquire their volatile elements. If the result holds, it suggests that the planet's bulk carbon and oxygen came largely from dust and ice solids rather than from disk gas, or that the disk gas became carbon-enriched only after the planet formed.

What carries the argument

Atmospheric retrieval with the petitRADTRANS package applied to the KPIC high-resolution spectrum, with the pressure-temperature profile fixed to a cloudless Sonora model at Teff = 1100 K and log g = 4.5 and with v sin i fixed to zero. The C/O and [C/H] values are constrained by the relative line depths of CO and H2O in spectral orders 31–33 of NIRSPEC, using a nested-sampling fit over radial velocity, quench pressure, and planet flux.

What would settle it

A higher-signal-to-noise spectrum of PDS 70b analyzed with a retrieval that lets clouds, the pressure-temperature profile, and v sin i vary freely would either confirm or overturn the stellar-like C/O; alternatively, a detection of refractory elements like Fe or silicates in the planet's atmosphere would discriminate between the solid-dominated and late-enrichment scenarios.

Watch

Extended reading notes

Core claim

The paper establishes that PDS 70b's atmosphere contains CO and H2O, detected via cross-correlation at combined significance of about 4.2σ, and derives a carbon-to-oxygen ratio of 0.28+0.20-0.12 (upper limit 0.63 at 95% confidence) and a metallicity [C/H] of -0.2+0.8-0.5 dex. These values are consistent with the host star PDS 70 A, whose C/O is about 0.44, and clearly lower than the gas-phase C/O of the outer disk inferred from ALMA to be ≳1. The authors also report a spin upper limit of <29 km/s for the planet. They interpret the stellar-like C/O as evidence that the planet's volatile budget is dominated by solids rather than gas, or that the disk underwent late carbon enrichment after the planet formed.

Load-bearing premise

The retrieval assumes a cloudless, non-rotating atmosphere with a pressure-temperature profile fixed to a model at 1100 K; if the real atmosphere has clouds, a different temperature structure, or significant rotation, the inferred carbon-to-oxygen ratio would shift.

Editorial extensions

If this is right

  • If the stellar-like C/O is real, the bulk carbon and oxygen of PDS 70b must have been delivered mostly by dust and ice aggregates rather than by the carbon-rich gas of the outer disk.
  • Alternatively, the disk gas became carbon-enriched after PDS 70b finished accreting, as predicted by models of disk chemical evolution and observed in some old disks.
  • The spin non-detection (<29 km/s) supports the picture that the planet is still contracting and has not yet undergone the spin-up phase expected after accretion ends.
  • Future higher-SNR observations of PDS 70b and PDS 70c, and measurements of isotope ratios such as 12C/13C and 16O/18O, could distinguish the dust-and-ice scenario from the late carbon-enrichment scenario.
  • A star-only model for the observed spectra is highly disfavored, supporting that the detected CO and H2O lines truly come from the planet atmosphere.

Reading between the lines

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

  • If this measurement holds, it implies that a planet's C/O ratio can stay stellar-like even when its surrounding disk is carbon-rich, so disk gas composition alone may not predict the composition of the forming planet.
  • The late carbon-enrichment interpretation predicts that planets forming early in a disk's lifetime should have stellar-like C/O, while those forming later, after carbon enrichment, would show superstellar C/O; a survey of protoplanets at different disk evolutionary stages would test this.
  • Measuring refractory species such as Fe or silicates in PDS 70b would break the degeneracy between the two scenarios without needing extreme signal-to-noise, because a dust-and-ice dominated accretion history should show enhanced refractory abundances.
  • A similar C/O measurement for the outer companion PDS 70c would test whether accretion chemistry varies with orbital radius inside the same disk.
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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

2 major / 3 minor

Summary. This Letter reports Keck/KPIC high-resolution spectroscopy of the protoplanet PDS 70b, with cross-correlation detections of CO (3.8 sigma) and H2O (3.5 sigma), a combined detection significance of 4.2 sigma, and an upper limit on the projected rotational velocity of v sin i < 29 km/s. The authors use a petitRADTRANS atmospheric retrieval to derive C/O = 0.28+0.20-0.12 (<0.63 at 95% confidence) and [C/H] = -0.2+0.8-0.5 dex, which they compare with the host star's C/O of 0.44 +/- 0.19 and the outer disk's gas-phase C/O of greater than or approximately 1. They conclude that PDS 70b's C/O is stellar-like and not gas-like, and discuss two formation scenarios: solid-dominated accretion or late carbon enrichment of the disk gas.

Significance. If correct, this is the first abundance measurement of a protoplanet embedded in its natal disk, a unique and important result for planet formation theory. The detection is supported by a very strong model comparison between a star-only and a star-plus-planet model (log10 Bayes factor 344.9, delta chi-square 772), which addresses the concern that the signal could be residual starlight. The paper is also honest about its limitations, explicitly acknowledging the noisy spectra and the need for future verification. The central abundance claim, however, rests on a fixed, cloudless thermal profile that the authors' own forward modeling disfavors, so the reported C/O should be treated as model-dependent unless its robustness is demonstrated.

major comments (2)
  1. [Section 5, Table 2] The retrieval fixes the cloudless Sonora pressure-temperature profile at Teff = 1100 K and log g = 4.5, yet the same data analyzed with BT-Settl model grids in Section 4.2 yield Teff = 1003+134-75 K and log g = 4.7+0.5-0.6 and explicitly find the cloudless Sonora model to be a worse fit (log10 Bayes factor = 0.7, 'substantial'). Because the C/O ratio is inferred from the relative strengths of CO and H2O lines, which form at pressure levels controlled by the thermal structure and cloud opacity, this choice could bias the derived C/O and its confidence interval. The manuscript should test the sensitivity of C/O and the 95% upper limit to (a) replacing the Sonora profile with the BT-Settl best-fit P-T profile, (b) including clouds, and (c) marginalizing over Teff and log g within the forward-model posterior.
  2. [Section 3, Section 5] The C/O and [C/H] constraints come from spectra with CO and H2O detections at only 3.8 sigma and 3.5 sigma, respectively. Given that the retrieval priors on C/O span 0.1-1.6, the reported median of 0.28 with an upper limit of 0.63 may be significantly prior-dependent. The authors should provide a quantitative comparison of the priors and posteriors for C/O and [C/H], for example by reporting the Hellinger distance or the information gain, so the reader can assess how much information the noisy KPIC spectra actually add beyond the assumed priors.
minor comments (3)
  1. [Section 4.2, Table 2] There is an inconsistency between the text and the table for the best-fit effective temperature: Section 4.2 reports Teff = 1003+134-75 K, while Table 2 lists Teff = 1103+134-75 K. Please correct the typo.
  2. [Section 7, Abstract] In Section 7, the text writes 'CO ∼ 0.44' when referring to the host star's carbon-to-oxygen ratio; this should be 'C/O ∼ 0.44' for clarity.
  3. [Section 4.2] The description of adding a 2.5 km/s systematic uncertainty to the radial velocity of PDS 70b is brief; please clarify whether this value was derived purely from Ruffio et al. (2023) or also from the observed RV scatter in this data, as it directly affects the claimed 2.5-sigma RV offset from the host star.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: C/O and [C/H] are free retrieval parameters fitted to the spectra, and the star/disk comparisons use external measurements.

full rationale

The central claims—C/O = 0.28+0.20-0.12 and [C/H] = -0.2+0.8-0.5—are produced by a petitRADTRANS retrieval in which C/O and [C/H] are free parameters with uniform priors (C/O uniform 0.1–1.6, [C/H] uniform -1.5 to 1.5), so the posteriors are not equal to the priors or to any input quantity by construction. The comparison values for the host star (C/O = 0.44 ± 0.19) and the outer disk (C/O ≳ 1) come from independent literature sources (Cridland et al. 2023; Facchini et al. 2021; Law et al. 2024), not from the same fit. The retrieval fixes a cloudless Sonora P-T profile at Teff = 1100 K and log g = 4.5, parameters informed by the same data's BT-Settl forward fit; this is a stated modeling assumption that could bias the inferred abundances, but it does not reduce the C/O claim to an input—C/O remains a free parameter and the posterior is data-driven. The paper also self-cites its own CCF and retrieval methodology (Wang et al. 2021c; Xuan et al. 2022; Hsu et al. 2024a), but these are code/method citations rather than load-bearing evidence for the physical result, and the methods are externally published and reproducible. No equation or derived quantity is equivalent to an input by construction, and no uniqueness theorem or ansatz is smuggled in via self-citation to force the conclusion. The acknowledged limitations—noisy spectra, fixed P-T profile, cloudless assumption—are correctness risks, not circularity.

Assumptions & free parameters 6 free parameters · 3 assumptions · 0 invented entities

The paper does not invent new physical entities. The central abundance result depends on a cloudless, 1D model atmosphere with a fixed P-T profile and on the accuracy of molecular opacities, both standard but not independently verified for PDS 70b.

free parameters (6)
  • C/O ratio = 0.28 +0.20/-0.12
    Retrieved carbon-to-oxygen ratio, the central claim of the paper.
  • Metallicity [C/H] = -0.2 +0.8/-0.5
    Retrieved carbon abundance relative to solar, used to support the stellar-like composition.
  • Quench pressure log Pquench = 1.6 +0.9/-0.8
    Pressure at which chemical quenching occurs in the retrieval model.
  • Projected rotational velocity v sin i = 9 +9/-7
    Best-fit value from forward model, consistent with non-detection; used to set upper limit <29 km/s.
  • Effective temperature Teff = 1103 +134/-75
    Best-fit from BT-Settl forward model, later fixed to 1100 K in the retrieval.
  • Surface gravity log g = 4.7 +0.5/-0.6
    Best-fit from forward model, later fixed to 4.5 in the retrieval.
assumptions (3)
  • domain assumption The atmosphere of PDS 70b is cloudless and described by the Sonora pressure-temperature profile at Teff=1100 K and log g=4.5.
    Section 5 states these are fixed in the retrieval; clouds would alter the molecular line strengths and the derived C/O.
  • domain assumption The stellar leakage into the planet fiber is well represented by the on-axis stellar spectrum of PDS 70 A.
    Section 4.2 fits a stellar template to the planet pointing; if the leakage has wavelength-dependent structure, the planet signal could be contaminated.
  • domain assumption Molecular opacities (CO, H2O, CH4) from HITEMP and Hargreaves et al. (2020) are accurate.
    The retrieval uses these line lists; inaccuracies would directly bias the abundance estimates.

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Cite this review

Pith. "Pith review of PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio." pith.science (2026). https://pith.science/paper/4QSYTRQW

@misc{pith2026241115117,
  author       = {Pith},
  title        = {Pith review of: PDS 70b Shows Stellar-like Carbon-to-oxygen Ratio},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4QSYTRQW}},
  note         = {Machine review of arXiv:2411.15117}
}
abstract

The $\sim$5 Myr PDS 70 is the only known system with protoplanets residing in the cavity of the circumstellar disk from which they formed, ideal for studying exoplanet formation and evolution within its natal environment. Here we report the first spin constraint and C/O measurement of PDS 70b from Keck/KPIC high-resolution spectroscopy. We detected CO (3.8 $\sigma$) and H$_2$O (3.5 $\sigma$) molecules in the PDS 70b atmosphere via cross-correlation, with a combined CO and H$_2$O template detection significance of 4.2 $\sigma$. Our forward model fits, using BT-Settl model grids, provide an upper limit for the spin-rate of PDS 70b ($<$29 km s$^{-1}$). The atmospheric retrievals constrain the PDS 70b C/O ratio to ${0.28}^{+0.20}_{-0.12}$ ($<$0.63 under 95$\%$ confidence level) and a metallicity [C/H] of ${-0.2}^{+0.8}_{-0.5}$ dex, consistent with that of its host star. The following scenarios can explain our measured C/O of PDS 70b in contrast with that of the gas-rich outer disk (for which C/O $\gtrsim$ 1). First, the bulk composition of PDS 70b might be dominated by dust+ice aggregates rather than disk gas. Another possible explanation is that the disk became carbon-enriched $\textit{after}$ PDS 70b was formed, as predicted in models of disk chemical evolution and as observed in both very low mass star and older disk systems with $\textit{JWST}$/MIRI. Because PDS 70b continues to accrete and its chemical evolution is not yet complete, more sophisticated modeling of the planet and the disk, and higher quality observations of PDS 70b (and possibly PDS 70c), are necessary to validate these scenarios.

Figures

Figures reproduced from arXiv: 2411.15117 by the authors.

Figure 1
Figure 1. Cross-correlation functions (CCFs) of our PDS 70b KPIC spectra against the molecular templates derived from the Sonora-Bobcat models. Upper : CCF (red solid line) of our KPIC spectra for the CO molecular templates. The stellar barycentric-included RV is depicted by the grey vertical dashed line. The auto-correlation function (ACF) of the CO molecular templates, normalized to the peak of CCF, is plotted as a dashed r… view at source ↗
Figure 2
Figure 2. KPIC spectrum of PDS 70b and its best-fit forward model using the BT-Settl model grids. The spectra were taken on 2024 May 23 (UT). Orders 31–33 on fiber 4 are shown in black lines. The full forward model, with the stellar speckle and planet fluxes, is in cyan lines. The stellar model, directly from the observed on-axis KPIC spectrum of PDS 70 A, is shown in blue lines. The planet model, including the best-fit BT-Se… view at source ↗
Figure 3
Figure 3. Top: Posteriors of the derived physical parame￾ters of PDS 70b using the BT-Settl models, including effec￾tive temperature, surface gravity, projected rotational and radial velocities. See Section 4.2 for details. Bottom: The posteriors of RV, C/O ratio and metallicity [C/H] derived from KPIC spectra of PDS 70b using the petitRADTRANS re￾trieval framework. See Section 5 for details. sible to constrain with the curre… view at source ↗

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