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arxiv: 2607.00973 · v1 · pith:UNV5V7Y4new · submitted 2026-07-01 · 🌌 astro-ph.EP

Transmission Spectrum of the Benchmark Temperate Exo-Neptune TOI-1231 b

Subhajit Sarkar , Nikku Madhusudhan , Lorenzo Pica-Ciamarra , M{\aa}ns Holmberg , Frances E. Rigby , Julianne I. Moses , Megan Mealing This is my paper

Pith reviewed 2026-07-02 05:27 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords transmission spectroscopyexoplanet atmospheresJWSTmethanecarbon dioxideTOI-1231 bmini-Neptunesub-Neptune
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The pith

JWST spectrum of TOI-1231 b detects methane and carbon dioxide consistent with a deep hydrogen-rich atmosphere.

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

The paper reports the first JWST transmission spectrum of the temperate exo-Neptune TOI-1231 b using NIRISS and NIRSpec data. It finds strong statistical evidence for methane and moderate evidence for carbon dioxide while placing high upper limits on ammonia, carbon monoxide, and sulfur species. A sympathetic reader would care because the planet's density already requires a thick hydrogen envelope, so its measured composition provides an empirical reference point for distinguishing mini-Neptune models from other sub-Neptune scenarios.

Core claim

We report a strong detection of CH4 (ln B = 54.5-69.6) and moderate to strong evidence for CO2 (ln B = 2.9-6.6). We do not find significant evidence for any other prominent molecule, although we find high 95% upper limits on the mixing ratios of NH3 and CO. This composition is consistent with expectations for a temperate Neptune possessing a deep H2-rich atmosphere with no distinct surface.

What carries the argument

Atmospheric retrieval analysis applied to the combined NIRISS and NIRSpec transmission spectrum that computes Bayesian evidence for individual molecular species.

If this is right

  • The absence of sulfur species distinguishes this planet from some other temperate sub-Neptunes.
  • High upper limits on ammonia and carbon monoxide align with predictions for deep hydrogen atmospheres.
  • The result supplies an empirical anchor for theoretical predictions of compositional differences between shallow and deep atmosphere scenarios.
  • It supports the mini-Neptune interpretation over hycean or gas-dwarf alternatives for this specific target.

Where Pith is reading between the lines

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

  • Similar retrievals on other density-confirmed temperate Neptunes could test whether methane-plus-carbon-dioxide signatures are common.
  • If future data on additional targets reproduce this pattern, interior models that predict distinct surfaces may need revision for the broader sub-Neptune population.

Load-bearing premise

The planet's measured bulk density is interpreted as requiring a thick hydrogen-rich atmosphere with no distinct surface.

What would settle it

A higher-precision spectrum that instead shows strong ammonia absorption or sulfur-bearing species at abundances above the current upper limits.

Figures

Figures reproduced from arXiv: 2607.00973 by Frances E. Rigby, Julianne I. Moses, Lorenzo Pica-Ciamarra, M{\aa}ns Holmberg, Megan Mealing, Nikku Madhusudhan, Subhajit Sarkar.

Figure 1
Figure 1. Figure 1: White light curves for transits of TOI-1231 b observed with two JWST instruments at different epochs. Left: NIRISS. Right: NIRSpec. In each case top panel shows light curve with best fit model (red line), while the bottom panel shows the residuals. Spot crossing events are evident in both the light curves. The white light curves shown here are from the JexoPipe reduction and are binned to one point every 1… view at source ↗
Figure 2
Figure 2. Figure 2: The transmission spectrum of TOI-1231 b. The observed JWST spectrum and retrieved model fits are shown for the fiducial retrieval using the JexoPipe data, considering the six prominent CNO molecules, with a single offset and no stellar heterogeneity, as discussed in Section 3. For visual clarity, the data shown here have been binned to R∼50. A retrieved offset of 79.38 ppm has been added to the NIRSpec dat… view at source ↗
Figure 3
Figure 3. Figure 3: Transmission spectra for NIRISS and NIRSpec from the two pipelines used in this study: JexoPipe and JExoRES. The spectra are binned to R∼50 for visual clarity. The grey line indicates the median retrieved spectrum from [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Posterior distributions for the abundances of the six molecular species included in our fiducial retrievals with a single offset, both with (indicated by a ⋆ symbol) and without stellar heterogeneity for JexoPipe, and with stellar heterogeneity included for JExoRES. The median retrieved values and 1σ error bars are shown for CH4 and CO2, while arrows indicate the 95% upper limits for all other species. log… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the posterior distributions for the abundances of all 11 molecules in the M23-informed set-up discussed in Section 3.3, as well as the temperature at 1µbar. We compare results for TOI-1231 b (blue) and K2-18 b (orange). The K2-18 b posteriors correspond to a new retrieval conducted in this work, using the same model and assumptions applied to TOI-1231 b. The median retrieved values and 1σ err… view at source ↗
Figure 6
Figure 6. Figure 6: Corner plot for the six-molecule model including one offset and no stellar heterogeneity, using the JexoPipe data [PITH_FULL_IMAGE:figures/full_fig_p019_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Corner plot for the six-molecule model including one offset and also stellar heterogeneity, using the JExoRES data [PITH_FULL_IMAGE:figures/full_fig_p020_7.png] view at source ↗
read the original abstract

The JWST is revolutionizing our understanding of the temperate sub-Neptune population through atmospheric spectroscopy. The nature of these planets remains debated, as their bulk properties are compatible with a range of interior scenarios, including mini-Neptunes, hycean worlds, and gas dwarfs, with different predicted atmospheric compositions. While theoretical studies have predicted compositional diagnostics for shallow- versus deep-atmosphere scenarios, there is a critical need for empirical constraints for a temperate planet that is a priori known to possess a deep H$_2$-rich atmosphere. The temperate exo-Neptune TOI-1231 b provides one such benchmark target. In this work, we present the JWST near-infrared (0.65--5.2 $\mu$m) transmission spectrum of TOI-1231 b, observed with NIRISS single-object slitless spectroscopy and NIRSpec G395H, representing the first for a temperate exo-Neptune. The density of TOI-1231 b requires a thick H$_2$-rich atmosphere, making the planet a keystone reference case for testing mini-Neptune scenarios for sub-Neptunes. We report a strong detection of CH$_4$ ($\ln B = 54.5$-$69.6$) and moderate to strong evidence for CO$_2$ ($\ln B = 2.9$-$6.6$). We do not find significant evidence for any other prominent molecule, although we find high 95\% upper limits on the mixing ratios of NH$_3$ and CO, both of which are expected in deep H$_2$-rich atmospheres. We also do not find any significant evidence for sulfur-bearing species that have been inferred for some temperate sub-Neptunes. This composition is consistent with expectations for a temperate Neptune possessing a deep H$_2$-rich atmosphere with no distinct surface. We discuss the implications of our results for the characterization of temperate sub-Neptunes.

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

0 major / 3 minor

Summary. The paper presents the first JWST near-infrared (0.65-5.2 μm) transmission spectrum of the temperate exo-Neptune TOI-1231 b, obtained with NIRISS single-object slitless spectroscopy and NIRSpec G395H. It reports a strong detection of CH4 (ln B = 54.5-69.6) and moderate to strong evidence for CO2 (ln B = 2.9-6.6), with no significant detections of other molecules including NH3, CO, or sulfur-bearing species, and high 95% upper limits on the latter two. The observed composition is interpreted as consistent with expectations for a deep H2-rich atmosphere with no distinct surface, establishing the planet as a benchmark reference for testing mini-Neptune scenarios for sub-Neptunes given its density-implied thick envelope.

Significance. If the retrieval results are robust, this work supplies a key empirical benchmark for temperate sub-Neptunes with confirmed deep H2 envelopes, directly addressing the need for observational constraints on compositional diagnostics predicted by theory. The high Bayesian evidence for CH4 constitutes a clear, high-significance detection in a challenging observational regime and provides falsifiable reference points for atmospheric chemistry models of similar planets.

minor comments (3)
  1. [Abstract] Abstract: the reported ranges for ln B (CH4: 54.5-69.6; CO2: 2.9-6.6) are presented without explanation of their origin (e.g., different data subsets, retrieval configurations, or model variants); this should be clarified in the main text or methods to allow readers to assess robustness.
  2. [Methods/Retrieval Setup] The manuscript should explicitly state the number of free parameters and priors used in the atmospheric retrievals (even if standard) to facilitate direct comparison with other JWST sub-Neptune studies.
  3. [Figures] Figure captions and axis labels for the transmission spectrum should clearly demarcate the NIRISS versus NIRSpec G395H wavelength coverage and note any overlapping regions or stitching procedures.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive summary and recommendation of minor revision. No major comments were provided in the report, so we have no specific points to address point-by-point. We will incorporate any minor suggestions from the full report in the revised manuscript.

Circularity Check

0 steps flagged

No significant circularity; empirical result from JWST data and standard retrievals

full rationale

The paper presents an observational transmission spectrum of TOI-1231 b from NIRISS and NIRSpec G395H JWST data, with molecular detections (CH4 ln B = 54.5-69.6; CO2 ln B = 2.9-6.6) obtained via standard atmospheric retrieval methods. The claim that the planet possesses a thick H2-rich atmosphere is framed as a prior constraint from independent density measurements, not derived internally. No load-bearing steps reduce by the paper's own equations to fitted inputs, self-citations, or ansatzes; the central results are externally falsifiable against the public dataset and do not involve renaming known patterns or uniqueness theorems imported from prior author work. This is a self-contained observational analysis.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

With only the abstract available, the ledger is limited to standard domain assumptions in exoplanet spectroscopy; no explicit free parameters or invented entities are stated.

axioms (2)
  • domain assumption Standard assumptions in exoplanet atmospheric retrieval models are valid for interpreting the transmission spectrum.
    Invoked to convert observed spectrum into molecular mixing ratio constraints and to interpret non-detections.
  • standard math Bayesian evidence (ln B) thresholds reliably indicate detection significance.
    Used to claim strong CH4 detection and moderate CO2 evidence.

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