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arxiv: 2605.01012 · v1 · submitted 2026-05-01 · 🌌 astro-ph.EP · astro-ph.SR

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Chemistry and Isotope Ratios of Substellar Atmospheres in the β Pictoris Young Moving Group

Aurora Kesseli, Dimitri Mawet, Ignas Snellen, Jerry W. Xuan, Malena Rice, Rico Landman, Sam de Regt, Tomas Stolker, Yapeng Zhang, Yurou Liu

Authors on Pith no claims yet

Pith reviewed 2026-05-09 17:54 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords C/O ratioisotope ratiosatmospheric retrievalbrown dwarfsexoplanet formationβ Pictoris moving grouphigh-resolution spectroscopysubstellar objects
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The pith

The ~12 Jupiter-mass companion 2MASS J0249-0557 c shows C/O, metallicity and 12CO/13CO ratios matching two brown dwarfs in the same moving group, favoring gravitational collapse over core accretion.

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

The paper measures the chemical and isotopic makeup of a planetary-mass companion at the planet-brown-dwarf boundary using high-resolution spectra. It retrieves a C/O ratio of 0.57, slightly elevated metallicity, and a 12CO/13CO ratio near 95, then demonstrates that two benchmark brown dwarfs in the β Pictoris young moving group yield consistent values. This match, together with the companion's wide separation, indicates that the object most likely formed through gravitational collapse in the manner of a star. The uniform compositions also supply a reference set for the entire moving group. Future comparisons with the group's true planets can then test whether those planets formed differently.

Core claim

Retrievals from CRIRES+ spectra with petitRADTRANS and PyMultiNest give 2MASS J0249-0557 c a C/O ratio of 0.57±0.01, [M/H] of 0.18±0.05, and 12CO/13CO of 95+23/-17. The same procedure applied to 2MASSI J0443+0002 and SIPS J2000-7523 produces matching abundances. Combined with the companion's large orbital distance, the shared composition identifies gravitational collapse in a star-like manner as the most probable formation channel for this object at the planet-brown-dwarf boundary. The solar-like abundances further establish a baseline for the β Pictoris young moving group.

What carries the argument

Atmospheric retrieval of C/O ratio, metallicity and 12CO/13CO isotope ratio from high-resolution near-infrared spectra via the petitRADTRANS radiative-transfer code and PyMultiNest nested sampler.

If this is right

  • The three objects supply the first homogeneous atmospheric-composition set for substellar members of the β Pictoris young moving group.
  • These solar-like abundances provide a reference against which the atmospheres of the group's exoplanets can be compared.
  • Direct comparisons within the group can distinguish core-accretion from gravitational-collapse formation for its planetary members.
  • The measurements demonstrate that high-resolution spectroscopy can constrain formation pathways near the planet-brown-dwarf boundary.

Where Pith is reading between the lines

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

  • If the retrieved ratios hold under alternative modeling, the same technique could be applied to other young moving groups to locate the mass or separation threshold where formation channels switch.
  • Discrepancies between a planet's composition and the group baseline could reveal whether that planet accreted gas after the group formed or inherited its chemistry from the natal cloud.
  • The isotope ratio may serve as an additional discriminant if future models predict different 12CO/13CO preservation under collapse versus disk-accretion scenarios.

Load-bearing premise

The retrieval procedure returns the true atmospheric C/O, metallicity and carbon-isotope values without large systematic biases from the assumed temperature-pressure profile, cloud treatment or line-list completeness.

What would settle it

An independent retrieval performed with a different radiative-transfer code or molecular line list that returns a C/O ratio more than 0.1 away from 0.57 while keeping the same data would falsify the claimed compositional consistency.

Figures

Figures reproduced from arXiv: 2605.01012 by Aurora Kesseli, Dimitri Mawet, Ignas Snellen, Jerry W. Xuan, Malena Rice, Rico Landman, Sam de Regt, Tomas Stolker, Yapeng Zhang, Yurou Liu.

Figure 1
Figure 1. Figure 1: Cross-correlation function (CCF) of CO, H2O, and 13CO detection for the three targets. From the 13CO CCF alone, we obtain a significant detection of 13CO for 2MASSI J0443+0002, a moderate detection for 2MASS J0249-0557c, and no detection for SIPS J2000-7523. The cloud parameters themselves remain only weakly constrained. A flexible P-T profile parametrization can partially mimic the spectral effects of clo… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of using log(g) as prior for atmospheric retrieval and using mass as prior for 2MASS J0249-0557c. The result of using log(g) is shown in gray, and the result of using mass is shown in red. In the mass prior case, there is a preference for a condensate cloud model, so we included a weakly constrained condensate cloud model. In the log(g) prior retrieval, there is a preference for a cloudless mode… view at source ↗
Figure 3
Figure 3. Figure 3: Two orders of high-resolution spectra with the best-fit model overplotted in yellow for each target. The observation on the first day (September 21, 2022) is chosen for 2MASS J0249-0557 c. The wavelength range is selected to include the 12CO and 13CO bandheads view at source ↗
Figure 4
Figure 4. Figure 4: Best-fit low-resolution model spectrum of 2MASS J0249-0557c. The pink points with error bars show the archival photometry, while the light-gray points show the corresponding synthetic photometry of the best-fit model. 4. We did not include clouds in our models for these two targets because, as M9 brown dwarfs, they are un￾likely to be cloudy. The retrieval results for these two brown dwarfs are shown in Fi… view at source ↗
Figure 5
Figure 5. Figure 5: Substellar objects with known 12CO/13CO, ex￾cluding the hot Jupiters. Literature values are shown in gray (Gandhi et al. 2023; Costes et al. 2024; Mulder et al. 2025; Gandhi et al. 2025; de Regt et al. 2024; Xuan et al. 2024a,b; Zhang et al. 2024; Gonz´alez Picos et al. 2024, 2025b; Grasser et al. 2025; Molli`ere et al. 2025; Wang et al. 2026). Values from this work are shown in color. The solar value of 8… view at source ↗
Figure 6
Figure 6. Figure 6: Corner plots of log(13CO/12CO), C/O, and [M/H] of the three targets in this study. The C/O ratios of all three targets are consistent with the solar abundance range of 0.59 ± 0.08 (Asplund et al. 2021). The CO iso￾topologue ratio distribution of SIPS J2000-7523 cannot be robustly determined as we do not have a strong detection of 13CO for this object (see Section 5.3). in Section 5.3, we do not have a sign… view at source ↗
Figure 7
Figure 7. Figure 7: C/O ratio and metallicity of objects in the β Pic Moving Group. Values and sources are shown in view at source ↗
read the original abstract

Measuring the chemical and isotopic compositions of gas giants and brown dwarfs provides insights into their formation pathways and birth environments. 2MASS J0249-0557 c is an L2-type planetary mass companion ($\sim 12 M_{\mathrm{Jup}}$) orbiting a pair of brown dwarfs in the $\beta$ Pictoris young moving group. Its mass places it at the intersection of planets and brown dwarfs, making it an interesting target for constraining formation pathways at the planet-brown-dwarf boundary. Using high-resolution spectroscopic data of the planet acquired with CRIRES+ mounted on VLT, we conduct atmospheric retrieval with the radiative transfer code \texttt{petitRADTRANS} and the nested sampling tool PyMultiNest. We retrieve a C/O ratio of $0.57\pm0.01$, a metallicity of [M/H] = $0.18\pm0.05$, and a $^{12}$CO/$^{13}$CO ratio of $95^{+23}_{-17}$. We also retrieve atmospheric compositions for two benchmark brown dwarfs in the $\beta$ Pic YMG, 2MASSI J0443+0002 and SIPS J2000-7523, using CRIRES+ data and find consistent compositions. Together with 2MASS J0249-0557 c's wide separation from its host, its compositional consistency with other members of its group supports gravitational collapse in a star-like manner as its most likely formation mechanism. These results deliver a homogeneous comparison of three substellar members in the $\beta$ Pic YMG. Their solar-like abundances provide a baseline for exoplanet members in the same moving group, such as $\beta$ Pic b, 51 Eri b, and AF Lep b, whose host stellar compositions are difficult to measure. Future comparisons of atmospheric compositions among this moving group offer the potential to distinguish between formation mechanisms for its planetary members.

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

1 major / 2 minor

Summary. The manuscript reports atmospheric retrievals from CRIRES+ high-resolution spectra for the ~12 M_Jup companion 2MASS J0249-0557 c and two brown dwarfs in the β Pictoris young moving group. Using petitRADTRANS and PyMultiNest, it finds C/O = 0.57 ± 0.01, [M/H] = 0.18 ± 0.05, and 12CO/13CO = 95^{+23}_{-17} for the companion, consistent with the brown dwarfs. Combined with its wide separation, this is interpreted as evidence for gravitational collapse formation, providing a baseline for other planets in the group.

Significance. If the retrievals prove robust, the work would be significant for constraining formation pathways at the planet-brown dwarf boundary through direct compositional comparison within a single young moving group. The homogeneous analysis across three substellar objects is a clear strength, establishing solar-like abundances as a reference point for exoplanets such as β Pic b, 51 Eri b, and AF Lep b whose host compositions are harder to measure.

major comments (1)
  1. [Atmospheric retrievals and results sections] The central claim that compositional consistency supports gravitational collapse (stated in the abstract) is load-bearing on the retrieved C/O, [M/H], and 12CO/13CO values being free of large correlated systematics. The manuscript applies the identical petitRADTRANS + PyMultiNest setup, including the same fixed T-P profile parametrization and cloud treatment, to the companion and both benchmark brown dwarfs. Any bias from these shared assumptions (e.g., line-list incompleteness or cloud modeling) would affect all three objects similarly, rendering the reported consistency expected by construction rather than an independent constraint on formation. The small formal uncertainties do not capture this model-dependence risk.
minor comments (2)
  1. The abstract gives asymmetric uncertainties on the 12CO/13CO ratio; the full text should explicitly state how these are extracted from the posterior (e.g., 16th/84th percentiles or highest-density interval).
  2. A side-by-side table of all retrieved parameters (with uncertainties) for the three objects would improve readability and facilitate the homogeneous comparison emphasized in the abstract.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and positive review, which highlights both the potential significance of the work and an important caveat regarding model assumptions. We address the major comment in detail below and have incorporated revisions to strengthen the discussion of limitations.

read point-by-point responses

  1. Referee: The central claim that compositional consistency supports gravitational collapse (stated in the abstract) is load-bearing on the retrieved C/O, [M/H], and 12CO/13CO values being free of large correlated systematics. The manuscript applies the identical petitRADTRANS + PyMultiNest setup, including the same fixed T-P profile parametrization and cloud treatment, to the companion and both benchmark brown dwarfs. Any bias from these shared assumptions (e.g., line-list incompleteness or cloud modeling) would affect all three objects similarly, rendering the reported consistency expected by construction rather than an independent constraint on formation. The small formal uncertainties do not capture this model-dependence risk.

    Authors: We agree that the identical retrieval framework introduces the possibility of correlated systematics, as any bias from the shared T-P profile parametrization, cloud treatment, or line lists would propagate similarly across all three objects. This means the reported compositional consistency is not fully independent and cannot, by itself, serve as a robust standalone constraint on formation pathways. The formal uncertainties reported are indeed statistical and do not encompass model systematic errors. However, the retrievals remain data-driven fits to independent spectra, and the convergence to solar-like values across objects with different effective temperatures and surface gravities still provides supporting context when combined with the companion's wide separation (an independent dynamical indicator favoring gravitational collapse). We will revise the manuscript to add an explicit discussion of these model-dependent risks, temper the language in the abstract and conclusions to present compositional consistency as one supporting element rather than primary evidence, and include a new paragraph on how shared assumptions limit the strength of the formation interpretation. revision: partial

Circularity Check

0 steps flagged

No circularity: retrieval outputs are independent of formation claim

full rationale

The paper applies standard atmospheric retrieval (petitRADTRANS + PyMultiNest) to independent CRIRES+ spectra of three distinct objects, producing C/O, [M/H], and isotopic ratios as direct posterior outputs. These values are then compared empirically across objects; the consistency is not enforced by any equation, shared fit parameter, or self-referential definition. The formation-mechanism inference is an interpretive step resting on the retrieved numbers plus the object's wide separation, with no load-bearing self-citation or ansatz that reduces the result to its inputs by construction. The derivation chain remains self-contained against the observed spectra.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The central claim rests on the fidelity of the atmospheric retrieval, which introduces many free parameters for temperature structure, abundances, and clouds, plus standard assumptions of the radiative-transfer code.

free parameters (4)
  • C/O ratio
    Retrieved parameter whose value is reported as the main result
  • metallicity [M/H]
    Retrieved parameter whose value is reported as the main result
  • 12CO/13CO ratio
    Retrieved parameter whose value is reported as the main result
  • temperature-pressure profile parameters
    Multiple free parameters required by the retrieval model
axioms (2)
  • domain assumption petitRADTRANS radiative transfer accurately models the observed spectrum under the assumed conditions
    Invoked when fitting the CRIRES+ data
  • domain assumption PyMultiNest nested sampling recovers the true posterior distribution
    Standard assumption in retrieval analyses

pith-pipeline@v0.9.0 · 5692 in / 1615 out tokens · 39490 ms · 2026-05-09T17:54:34.672341+00:00 · methodology

discussion (0)

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