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The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase

T0 review · 3 major / 6 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read JWST spectroscopy shows a 34-million-year-old low-mass star still surrounded by a carbon-rich planet-forming gas disk.

desk verdict First JWST spectrum of a ~30 Myr disk is a real observational step forward; the carbon-rich conclusion is credible but the C/O>2 number is softer than the abstract implies. read the letter →

arxiv 2412.05535 v2 pith:YLNLIBXU submitted 2024-12-07 astro-ph.EP astro-ph.GAastro-ph.SR

Feng Long , Ilaria Pascucci , Adrien Houge , Andrea Banzatti , Klaus M. Pontoppidan , Joan Najita , Sebastiaan Krijt , Chengyan Xie
show 15 more authors
Joe Williams Gregory J. Herczeg Sean M. Andrews Edwin Bergin Geoffrey A. Blake María José Colmenares Daniel Harsono Carlos E. Romero-Mirza Rixin Li Cicero X. Lu Paola Pinilla David J. Wilner Miguel Vioque Ke Zhang the JDISCS collaboration
This is my paper · ORCID
classification astro-ph.EPastro-ph.GAastro-ph.SR
keywords protoplanetarydisksJWSTMIRI/MRSdiskchemistrycarbon-richhydrocarbonslifetimelow-massstarsC/Oratio
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 uses JWST mid-infrared spectroscopy to show that the inner disk around J0446B, an M4.5 star thought to be $\sim$34 Myr old, is filled with hydrocarbons—acetylene, benzene, methane, and many others—and almost no water. The detection of spatially unresolved molecular hydrogen and neon emission lines is read as evidence that this is a long-lived primordial gas disk, not a debris disk, making it the first confirmed case of disk gas surviving past 30 Myr. From the ratio of acetylene to carbon dioxide, the authors estimate a gas-phase carbon-to-oxygen ratio $\mathrm{C/O} \gtrsim 2$, so the inner disk is very carbon-rich. They argue this fits a picture in which low-mass stars deplete their icy pebbles early, pass through a water-rich phase, and end up carbon-rich while the disk slowly drains inward. If correct, the result extends the known lifetime of planet-forming gas disks by an order of magnitude and links late disk chemistry to the carbon content of planets forming around the smallest stars.

What carries the argument

The central object is the MIRI/MRS spectrum itself: continuum-subtracted mid-infrared data over 4.9–28.6 $\mu$m, fitted with LTE plane-parallel slab models that include optical-depth and line-overlap effects, producing column density, temperature, and emitting area for each molecule. Two derived ratios carry the chemical argument: the C$_2$H$_2$/CO$_2$ column-density ratio, converted to gas-phase $\mathrm{C/O}$ through thermo-chemical model grids, and the H$_2$ S(1)/S(3) line ratio, which yields the warm gas temperature. The time-evolution claim is carried by a 1D $\alpha$-disk model that tracks the inward drift and sublimation of icy pebbles and the accretion of outer carbon-rich gas, showing that a high inner $\mathrm{C/O}$ can be sustained for tens of Myr at $\alpha \lesssim 10^{-4}$.

What would settle it

A decisive check would be to resolve the H$_2$ and [Ne II] emission spatially or spectrally at higher angular and spectral resolution: if the lines are extended or systematically blueshifted, they trace a disk wind rather than a primordial disk. Independently, a lithium detection or a revised moving-group membership that puts J0446B at an age under $\sim$10 Myr would remove the '30-Myr-old disk' framing, and a direct measurement of the gas-phase $\mathrm{C/O}$ from another tracer (for example, ALMA observations of HCN or C$_2$H) that gives $\mathrm{C/O} < 1$ would undercut the carbon-rich claim.

Watch

Extended reading notes

Core claim

The paper's central claim is that J0446B is the first confirmed example of a primordial protoplanetary disk with gas surviving past $\sim$30 Myr, and that its inner disk has entered a late, hydrocarbon-dominated, carbon-rich phase. The evidence is a MIRI/MRS spectrum from 4.9 to 28.6 $\mu$m showing 14 molecular species, including nine hydrocarbons with a very optically thick C$_2$H$_2$ component, a marginal water detection, five pure-rotational H$_2$ lines, and spatially unresolved [Ne II] and [Ar II] lines. Slab-model column densities, mapped through thermo-chemical model grids, imply a gas-phase $\mathrm{C/O} \gtrsim 2$. The authors place J0446B at the oldest end of the JWST M-star disk sample, with hydrocarbon excitation conditions (T $\sim$ 250–300 K, emitting radii 0.05–0.1 AU) similar to younger carbon-rich disks, and use a 1D viscous disk model with pebble drift and volatile transport to argue that such a carbon-rich state can persist for tens of Myr only if the disk viscosity is low, $\alpha \lesssim 10^{-4}$.

Load-bearing premise

The argument assumes both that J0446B is truly $\sim$34 Myr old (with membership and lithium age taken from the literature rather than measured independently for this star) and that the unresolved H$_2$ and neon lines trace disk gas rather than a small-scale disk wind.

Editorial extensions

If this is right

  • If J0446B is truly a 34-Myr-old primordial disk, disk gas can survive roughly ten times longer than the canonical few-Myr disk lifetime, at least around very low-mass stars.
  • Planets forming in such a disk would accrete gas with $\mathrm{C/O} \gtrsim 2$, producing carbon-rich atmospheres with different chemistry and haze formation than solar-composition planets.
  • The millimeter-faint, carbon-rich disks around late M stars are expected to be the norm at ages beyond $\sim$10 Myr, while water-rich disks like Sz 114 are the exception, tied to bright millimeter emission and dust substructures that trap icy pebbles.
  • Maintaining the carbon-rich phase for tens of Myr requires a slowly evolving disk with $\alpha \lesssim 10^{-4}$, linking the observed chemistry to the disk's viscosity and lifetime.
  • The comparable fluxes of [Ne II] and [Ar II] imply soft X-ray/EUV ionization dominates, so stellar high-energy radiation alone may not disperse such disks.

Reading between the lines

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

  • The paper does not forecast how common long-lived carbon-rich disks are; a natural next step is a JWST survey of the known accreting M-dwarf disks at 20–50 Myr, measuring the fraction that are hydrocarbon-dominated. The pebble-drift picture predicts that fraction rises with age and anticorrelates with millimeter flux.
  • The carbon-rich inner disk implies carbon is being transferred from solids to gas; if this is general, terrestrial planets assembled late in such systems could be carbon-poor even while the gas they accrete is carbon-rich, a bias worth folding into interpretations of exoplanet atmospheric C/O for M-dwarf systems like TRAPPIST-1.
  • A testable extension of the low-viscosity requirement: high-spectral-resolution observations of CO or H$_2$ line profiles in J0446B could measure turbulence and constrain $\alpha$ directly, providing an independent check on the $\alpha \lesssim 10^{-4}$ limit inferred from chemistry.
  • The unresolved [Ne II] and [Ar II] lines could be used as a diagnostic in other old disks to tell whether stellar high-energy radiation or an unseen wind controls the final disk dispersal.
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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

3 major / 6 minor

Summary. The paper presents JWST MIRI/MRS 4.9–28.6 μm spectroscopy of J0446B, an M4.5 star in the ~34 Myr-old χ1 For association with weak accretion signatures. It reports the detection of 14 molecular species, dominated by hydrocarbons (CH4, C2H2, C2H4, C2H6, C6H6, etc.), plus H2 pure-rotational lines, [Ne II], and [Ar II], with only a marginal H2O detection. Slab-model fits yield a very high column density optically thick C2H2 component and a high N(C2H2)/N(CO2) ratio. Using the Najita et al. (2011) chemical grid, the authors infer a gas-phase C/O ≳2. They argue that the spatially unresolved H2 and [Ne II] emission indicates a long-lived primordial disk, and chemcomp models suggest that maintaining a carbon-rich inner disk for tens of Myr requires α-viscosity ≲1e-4. The paper interprets J0446B as the first detailed characterization of disk gas at ~30 Myr and as evidence for a late-stage carbon-rich phase in disk evolution.

Significance. If the claims hold, this is a significant observational advance: it extends the well-characterized gas-disk phase from ~10 Myr to ~30 Myr, presents the richest hydrocarbon inventory yet seen in an old disk, and connects the observed chemistry to pebble-drift/volatile-transport disk evolution. The strengths of the paper include the use of a published reduction pipeline, public JWST data, careful line identification with HITRAN/iSLAT, and explicit acknowledgment of several caveats (e.g., line-width scaling, model-grid limitations, unresolved wind alternative). The qualitative result that J0446B is molecule-rich and hydrocarbon-dominated appears credible and is well documented. However, the headline quantitative claim (C/O ≳2) and the primordial-disk classification are not yet as secure as the line detections themselves: systematic uncertainties in the slab-model columns and in the chemical-grid mapping are not propagated into the reported C/O, and the H2/[Ne II] unresolved detections do not uniquely exclude a disk wind. These issues are addressable with additional analysis and do not undermine the value of the observations themselves.

major comments (3)
  1. [§3.2, Table 1] The central claim of gas-phase C/O ≳2 (abstract; §4.3.1) is derived from N(C2H2)/N(CO2), where the numerator is dominated by the optically thick C2H2 component with log N = 22.54 ± 0.26 cm^-2. The text in §3.2 states that for optically thick lines the column density scales roughly inversely with the assumed Gaussian width σ = 2 km/s, and the table caption notes that the quoted uncertainties are statistical and likely underestimated. No systematic uncertainty is propagated for σ, for the continuum/pseudo-continuum placement (including the excluded 7.1–8.5 and 12.0–16.5 μm regions), or for the plane-parallel slab geometry. Since the ratio in Figure 6 is what is mapped to C/O, an unquantified factor of a few in the thick C2H2 column can shift the inferred C/O from ≳2 toward ~1. The authors should refit with σ = 3 and 4 km/s, vary the continuum level, and report the resulting range in N(C2H2)/N(CO2) and in C/O. In addition, part of the 'thick' pseudo-continuum could in principle be produced by the many blended hydrocarbon lines detected here; this degeneracy should be explicitly discussed and, if possible, tested with the full molecular inventory included in the fit.
  2. [§3.3 and §4.1] The statement in §4.1 that 'the detection of spatially unresolved H2 and [Ne II] lines strongly suggests that J0446B hosts a long-lived primordial gas disk' goes beyond what §3.3 establishes. The same section concedes that 'the possibility of tracing a small-scale unresolved disk wind cannot be completely ruled out, given the moderate spatial resolution of MIRI/MRS (0.2–0.3).' Since [Ne II] is routinely identified as a disk-wind/jet tracer (as the paper itself notes), the unresolved detection does not uniquely require a quasi-static primordial disk. The authors should provide a quantitative discriminator — for example, line-centroid shifts, flux ratios among the H2 transitions, or an upper limit on the emitting radius from the point-spread function — or should temper the 'first confirmed case' claim to say that the emission is consistent with primordial disk gas but an unresolved wind is not excluded.
  3. [§4.3.1, Figure 6] The conversion from N(C2H2)/N(CO2) to C/O relies on the Najita et al. (2011) chemical grid, which the text itself notes was developed for warmer T Tauri disks and does not include pathways to the complex hydrocarbons (C2H4, C2H6, C6H6, etc.) that dominate the observed spectrum. These two effects may act in opposite directions on the derived C/O, but they are not quantified, so the resulting 'C/O ≳2' is a model-dependent inference without a stated systematic error. The authors should test the mapping with a network that includes these species at intermediate C/O values (e.g., a Kanwar et al. 2024b-type grid with C/O = 1–4 for J0446B-like parameters) or otherwise provide a quantitative uncertainty on C/O from the grid choice. Without this, the abstract's headline number is not yet robust, even if the qualitative carbon-rich conclusion survives.
minor comments (6)
  1. [Table 1] The note that the uncertainties are 'statistical and likely underestimated' is important for the C/O derivation and should be repeated in the main text where the column densities are used, not only in the table footnote.
  2. [§4.3.1] The statement that 'the resulting C/O ratio is also close to 2 based on the column density ratio of C2H2 and H2O' is based on an upper limit for H2O; it should be phrased as a lower limit on C/O from water, not as a measurement.
  3. [Figure 6] The observed values/ranges plotted in the left panel lack visible error bars; since the x-axis is a model-derived quantity, the figure should include propagated uncertainties or state explicitly that they are omitted.
  4. [§2.1] The text first quotes the M6 spectral type from Silverberg et al. (2020) and then derives M4.5; please state explicitly that the adopted spectral type is M4.5 (Teff ≈ 3100 K) throughout the remainder of the paper to avoid confusion.
  5. [§4.1 and Abstract] The phrase 'first confirmed case of disk gas surviving for more than 30 Myr' is stronger than the abstract's 'first detailed characterization of disk gas at ~30 Myr'; consider harmonizing the wording given the unresolved-wind degeneracy.
  6. [§4.3.2, Figure 8] The conclusion that maintaining C/O > 1 at ~30 Myr requires α ≲ 1e-4 depends on the assumed initial volatile partitioning (60% refractory carbon, 20% CO, 10% CO2, 10% CH4) and v_frag = 5 m/s; the paper should state how sensitive Figure 8 is to these choices.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the C/O estimate is an external model-grid mapping of measured column ratios, and the evolutionary conclusions come from forward chemcomp runs, not from fitted parameters or self-citations.

full rationale

The paper's central claims are observationally anchored and not reduced to their inputs by construction. The detected species, line fluxes, and slab-model column densities are independent of the chemistry grids used for interpretation. The quantitative C/O ratio is obtained by mapping the measured N(C2H2)/N(CO2) column-density ratio onto the published thermo-chemical grid of Najita et al. (2011), which is an external model computed from stated assumptions (C/O from 0.2 to 4, solar 0.45) and not fitted to this spectrum; the paper explicitly notes caveats about the grid's T Tauri assumptions and cross-checks with the independent Kanwar et al. (2024b) models. The alpha-viscosity conclusion (alpha < 1e-4) is the output of forward chemcomp simulations matching stellar parameters, not a parameter fitted to the observed column ratios, so it is not a fitted input renamed as a prediction. The H2 and [Ne II] detections are direct spectroscopic measurements; interpreting them as evidence for primordial gas is an inference supported by external debris-disk non-detections, not a definitional equivalence. Self-citations exist (Najita et al. 2011; Mah et al. 2023), but they are not load-bearing in the prohibited sense: the cited models are external, parameter-free with stated assumptions, and the present paper runs its own evolutionary calculations rather than importing the conclusion. The acknowledged systematic sensitivity of the optically thick C2H2 column to the assumed 2 km/s line width is a model-dependence/correctness concern, not a circularity, because no equation in the paper defines the claimed C/O in terms of that assumption. No step reduces the central claim to its inputs by construction, so the appropriate finding is no significant circularity.

Assumptions & free parameters 11 free parameters · 6 assumptions · 0 invented entities

The paper is primarily an observational characterization; its central claims depend on a chain of modeling assumptions rather than on a mathematical derivation. Slab-model column densities are fitted to the spectrum, and the C/O inference is read from published chemical-model grids. The disk-evolution models introduce chosen initial conditions such as viscosity, disk mass, and volatile partitioning. No new physical entities are proposed; the optically thick C2H2 component is a modeling construct within the iris slab framework.

free parameters (11)
  • Slab-model column density N(C2H2), optically thick component = log N = 22.54 +/- 0.26 cm^-2
    Fitted to the 12-16 um pseudo-continuum; this column drives the high C2H2/CO2 ratio and hence the C/O >2 estimate.
  • Slab-model column density N(C2H2), thin component = log N = 18.36 +/- 0.05 cm^-2
    Fitted to C2H2 lines; used together with CO2 for the alternate C/O inference.
  • Slab-model column density N(CO2) = log N = 18.46 +/- 0.17 cm^-2
    The main oxygen-bearing molecule; the C2H2/CO2 column ratio is mapped to C/O through Najita et al. (2011) grids.
  • Slab-model excitation temperature and emitting radius for each molecule = T = 170-309 K, Rslab = 0.02-1.1 AU (Table 1)
    Each molecule is fit with three parameters (N, T, A); these determine the column densities used in the C/O estimate.
  • Gaussian line width sigma = 2 km/s
    Assumed for all slab models to match previous studies; optically thick column densities scale inversely with line width.
  • Wavelength-dependent continuum offset at >16.5 um = small offset from Banzatti et al. (2024) line-free regions
    Applied to better match the expected continuum in the water region; affects the marginal H2O detection and line ratios.
  • chemcomp alpha-viscosity = explored 5e-4, 1e-4, 1e-5; conclusion requires <1e-4
    Viscosity is an input to disk evolution models; the statement that a high C/O ratio persists to 30 Myr depends on the low-alpha branch.
  • Initial disk mass in chemcomp models = 1%, 10%, and 25% of stellar mass
    Scanned to test the sensitivity of C/O evolution; the qualitative low-alpha conclusion is robust across these values.
  • Initial carbon volatile partitioning = 60% refractory C, 20% CO, 10% CO2, 10% CH4
    Adopted from Mah et al. (2023) as an input to chemcomp; changes the timing and amplitude of C/O evolution.
  • Dust fragmentation velocity v_frag = 5 m/s
    Input to the Birnstiel et al. (2012) two-population dust model; affects pebble drift speed and the C/O timeline.
  • Initial characteristic disk radius R_c = 55 AU
    Set to match measured disk sizes around very low-mass stars; affects viscous and pebble drift timescales.
assumptions (6)
  • domain assumption J0446B is a member of the chi1 For association with age 33.7 Myr.
    Adopted in Section 2.1 from Luhman (2024) based on Gaia DR3 membership and lithium depletion; the old-age framing depends on it.
  • domain assumption The observed unresolved H2 and [Ne II] emission originates in disk gas rather than an unresolved disk wind.
    Section 3.3 states the wind cannot be completely ruled out; Section 4.1 uses these lines as the primary evidence for a primordial disk.
  • domain assumption Plane-parallel LTE slab models with a single temperature, column, and area adequately represent the emitting gas.
    Section 3.2 adopts the iris slab model; the derived column densities and C/O ratio inherit this assumption.
  • domain assumption The Najita et al. (2011) thermo-chemical model grid, developed for warmer T Tauri disks, maps observed C2H2/CO2 column ratios to gas-phase C/O.
    Section 4.3.1 uses this grid to estimate C/O >2; the paper lists caveats about temperature and incomplete hydrocarbon networks.
  • domain assumption The chemcomp model (Schneider & Bitsch 2021), with the stated initial volatile distribution, captures the long-term C/O evolution of the disk.
    Section 4.3.2 uses chemcomp results to argue that alpha < 1e-4 is required for a C-rich state at 30 Myr.
  • domain assumption HITRAN line lists used for molecule identification and slab modeling are complete and accurate for the fitted bands.
    Section 3.2 uses HITRAN; the paper notes 13CCH2 line data are incomplete, so some column densities are uncertain.

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Cite this review

Pith. "Pith review of The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase." pith.science (2026). https://pith.science/paper/YLNLIBXU

@misc{pith2026241205535,
  author       = {Pith},
  title        = {Pith review of: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YLNLIBXU}},
  note         = {Machine review of arXiv:2412.05535}
}
abstract

We present a JWST MIRI/MRS spectrum of the inner disk of WISE J044634.16$-$262756.1B (hereafter J0446B), an old ($\sim$34 Myr) M4.5 star but with hints of ongoing accretion. The spectrum is molecule-rich and dominated by hydrocarbons. We detect 14 molecular species (H$_2$, CH$_3$, CH$_4$, C$_2$H$_2$, $^{13}$CCH$_2$, C$_2$H$_4$, C$_2$H$_6$, C$_3$H$_4$, C$_4$H$_2$, C$_6$H$_6$, HCN, HC$_3$N, CO$_2$ and $^{13}$CO$_2$) and 2 atomic lines ([Ne II] and [Ar II]), all observed for the first time in a disk at this age. The detection of spatially unresolved H$_2$ and Ne gas strongly supports that J0446B hosts a long-lived primordial disk, rather than a debris disk. The marginal H$_2$O detection and the high C$_2$H$_2$/CO$_2$ column density ratio indicate that the inner disk of J0446B has a very carbon-rich chemistry, with a gas-phase C/O ratio $\gtrsim$2, consistent with what have been found in most primordial disks around similarly low-mass stars. In the absence of significant outer disk dust substructures, inner disks are expected to first become water-rich due to the rapid inward drift of icy pebbles, and evolve into carbon-rich as outer disk gas flows inward on longer timescales. The faint millimeter emission in such low-mass star disks implies that they may have depleted their outer icy pebble reservoir early and already passed the water-rich phase. Models with pebble drift and volatile transport suggest that maintaining a carbon-rich chemistry for tens of Myr likely requires a slowly evolving disk with $\alpha-$viscosity $\lesssim10^{-4}$. This study represents the first detailed characterization of disk gas at $\sim$30 Myr, strongly motivating further studies into the final stages of disk evolution.

Figures

Figures reproduced from arXiv: 2412.05535 by the authors.

Figure 1
Figure 1. The spectral energy distribution of J0446B including the JWST MIRI/MRS spectrum in blue (the noisy long￾wavelength range is marked with lighter color). The grey curve shows a stellar photospheric model with Teff = 3100 K (Allard et al. 2012). The four WISE band photometry encompassed both stellar components in the binary system of J0446; the triangles represent the contribution of J0446B to W1 and W2 bands assuming … view at source ↗
Figure 2
Figure 2. Top: The MIRI-MRS spectrum (black) of the disk of J0446B and the estimated continuum emission (orange). The shorter wavelength affected by stellar absorption and the wavelength range longer than 18 µm with worse data quality and no lines-of-interest are cut out. The identified molecules are marked out. Bottom: The continuum-subtracted spectrum (grey), where the regions with pseudo-continuum emission from the optical… view at source ↗
Figure 3
Figure 3. The comparison of data and model spectra. Top panels: The continuum-subtracted data spectrum (black) with a model spectrum (orange-shaded region) composed of all fitted species. The optically thick emission of C2H2 is highlighted in light blue. Bottom panels: Model spectra for individual molecules in each wavelength segment. The insert plot highlights the marginal detection of H2O, and the possible detection of emis… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Left: Zoomed-in spectra around molecular hydrogen pure rotational lines. Fitted Gaussian profiles are overplotted for detected lines. H2 S(2), S(4), S(5) are blended with hydrocarbon emissions, for which the slab models are indicated in blue with the original data spec…
Figure 5
Figure 5. Figure 5: Left: the 17.22 µm water line luminosity vs. C2H2 Q-branch line luminosity for a mixed sample from JWST and Spitzer; Right: the 17.22 µm water line luminosity vs. C2H2 to water flux ratio. The M star sample refers stars with spectral type later than M3, and is labelled…
Figure 6
Figure 6. Figure 6: Left: The input gas C/O ratio vs. the output column density ratio of C2H2 and CO2 from Najita et al. (2011) chemical models (connected grey dots). The observed values/ranges of the JWST mid-to-late M-star disk sample are highlighted in colors, except for Sz 28, for whi…
Figure 7
Figure 7. Figure 7: Left: stellar age vs. C2H2 to water flux ratio for the mid-to-late M disk sample, using the same target labelling as [PITH_FULL_IMAGE:figures/full_fig_p013_7.png]
Figure 8
Figure 8. Figure 8: The modelled time evolution of gas-phase C/O ratio using chemcomp (Schneider & Bitsch 2021) in a disk around a very low-mass star, with stellar properties consis￾tent with J0446B. The line styles represent different α viscos￾ity and the line colors represent different …
Figure 9
Figure 9. Figure 9: Left: The spectral energy distribution of J0446A including the JWST MIRI/MRS spectrum in blue (the noisy long￾wavelength range is marked with lighter color). The grey curve shows a stellar photospheric model with Teff = 3100 K. The VISTA J-band flux of J0446A might be …
Figure 10
Figure 10. Figure 10: The observed spectrum (black) in comparison with CO (orange) and H2O (blue) models (scaled) with emitting temperature of 3100 K. Boucher, A., Lafreni`ere, D., Gagn´e, J., et al. 2016, ApJ, 832, 50, doi: 10.3847/0004-637X/832/1/50 Busso, G., Cacciari, C., Bellazzini, M…
Figure 11
Figure 11. Figure 11: Examples of unidentified lines (marked with “?”) in the MIRI/MRS spectrum of J0446B. Colmenares, M. J., Bergin, E., Salyk, C., et al. 2024, arXiv e-prints, arXiv:2410.18187, doi: 10.48550/arXiv.2410.18187 Cronin-Coltsmann, P. F., Kennedy, G. M., Kral, Q., et al. 2023,…

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Pith tools

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